lds_baseline.ipynb

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        "<a href=\"https://colab.research.google.com/github/manasi-ganti/long-doc-summarization-gpt/blob/main/lds_baseline.ipynb\" target=\"_parent\"><img src=\"https://colab.research.google.com/assets/colab-badge.svg\" alt=\"Open In Colab\"/></a>"
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          "text": [
            "Looking in indexes: https://pypi.org/simple, https://us-python.pkg.dev/colab-wheels/public/simple/\n",
            "Collecting sumy\n",
            "  Downloading sumy-0.10.0-py2.py3-none-any.whl (94 kB)\n",
            "\u001b[K     |████████████████████████████████| 94 kB 2.2 MB/s \n",
            "\u001b[?25hRequirement already satisfied: requests>=2.7.0 in /usr/local/lib/python3.7/dist-packages (from sumy) (2.23.0)\n",
            "Collecting pycountry>=18.2.23\n",
            "  Downloading pycountry-22.3.5.tar.gz (10.1 MB)\n",
            "\u001b[K     |████████████████████████████████| 10.1 MB 44.1 MB/s \n",
            "\u001b[?25h  Installing build dependencies ... \u001b[?25l\u001b[?25hdone\n",
            "  Getting requirements to build wheel ... \u001b[?25l\u001b[?25hdone\n",
            "    Preparing wheel metadata ... \u001b[?25l\u001b[?25hdone\n",
            "Collecting breadability>=0.1.20\n",
            "  Downloading breadability-0.1.20.tar.gz (32 kB)\n",
            "Requirement already satisfied: nltk>=3.0.2 in /usr/local/lib/python3.7/dist-packages (from sumy) (3.7)\n",
            "Collecting docopt<0.7,>=0.6.1\n",
            "  Downloading docopt-0.6.2.tar.gz (25 kB)\n",
            "Requirement already satisfied: chardet in /usr/local/lib/python3.7/dist-packages (from breadability>=0.1.20->sumy) (3.0.4)\n",
            "Requirement already satisfied: lxml>=2.0 in /usr/local/lib/python3.7/dist-packages (from breadability>=0.1.20->sumy) (4.9.1)\n",
            "Requirement already satisfied: joblib in /usr/local/lib/python3.7/dist-packages (from nltk>=3.0.2->sumy) (1.2.0)\n",
            "Requirement already satisfied: regex>=2021.8.3 in /usr/local/lib/python3.7/dist-packages (from nltk>=3.0.2->sumy) (2022.6.2)\n",
            "Requirement already satisfied: tqdm in /usr/local/lib/python3.7/dist-packages (from nltk>=3.0.2->sumy) (4.64.1)\n",
            "Requirement already satisfied: click in /usr/local/lib/python3.7/dist-packages (from nltk>=3.0.2->sumy) (7.1.2)\n",
            "Requirement already satisfied: setuptools in /usr/local/lib/python3.7/dist-packages (from pycountry>=18.2.23->sumy) (57.4.0)\n",
            "Requirement already satisfied: urllib3!=1.25.0,!=1.25.1,<1.26,>=1.21.1 in /usr/local/lib/python3.7/dist-packages (from requests>=2.7.0->sumy) (1.24.3)\n",
            "Requirement already satisfied: certifi>=2017.4.17 in /usr/local/lib/python3.7/dist-packages (from requests>=2.7.0->sumy) (2022.9.24)\n",
            "Requirement already satisfied: idna<3,>=2.5 in /usr/local/lib/python3.7/dist-packages (from requests>=2.7.0->sumy) (2.10)\n",
            "Building wheels for collected packages: breadability, docopt, pycountry\n",
            "  Building wheel for breadability (setup.py) ... \u001b[?25l\u001b[?25hdone\n",
            "  Created wheel for breadability: filename=breadability-0.1.20-py2.py3-none-any.whl size=21712 sha256=4944e53e181e1d8c649e5cb04bd545b19889bf60884db69b25e5ea9f579e1c31\n",
            "  Stored in directory: /root/.cache/pip/wheels/d4/bf/51/81d27ad638e1a6dca4f362ecc33d1e2c764b8ea7ec751b8fc1\n",
            "  Building wheel for docopt (setup.py) ... \u001b[?25l\u001b[?25hdone\n",
            "  Created wheel for docopt: filename=docopt-0.6.2-py2.py3-none-any.whl size=13723 sha256=c7c193c7834116607460d2606e767097f52be96e832d4497adfccaed72cb5d70\n",
            "  Stored in directory: /root/.cache/pip/wheels/72/b0/3f/1d95f96ff986c7dfffe46ce2be4062f38ebd04b506c77c81b9\n",
            "  Building wheel for pycountry (PEP 517) ... \u001b[?25l\u001b[?25hdone\n",
            "  Created wheel for pycountry: filename=pycountry-22.3.5-py2.py3-none-any.whl size=10681845 sha256=3abd4507be816048d424204200422eb6ca87f4b5210943df16bc40261d40a87b\n",
            "  Stored in directory: /root/.cache/pip/wheels/0e/06/e8/7ee176e95ea9a8a8c3b3afcb1869f20adbd42413d4611c6eb4\n",
            "Successfully built breadability docopt pycountry\n",
            "Installing collected packages: docopt, pycountry, breadability, sumy\n",
            "Successfully installed breadability-0.1.20 docopt-0.6.2 pycountry-22.3.5 sumy-0.10.0\n"
          ]
        }
      ],
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        "!python3 -m pip install sumy"
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        "outputId": "92cb811b-9de9-4028-f58c-3d62990ebf8c"
      },
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          "text": [
            "Looking in indexes: https://pypi.org/simple, https://us-python.pkg.dev/colab-wheels/public/simple/\n",
            "Collecting datasets\n",
            "  Downloading datasets-2.5.2-py3-none-any.whl (432 kB)\n",
            "\u001b[K     |████████████████████████████████| 432 kB 11.0 MB/s \n",
            "\u001b[?25hRequirement already satisfied: fsspec[http]>=2021.11.1 in /usr/local/lib/python3.7/dist-packages (from datasets) (2022.8.2)\n",
            "Requirement already satisfied: pyarrow>=6.0.0 in /usr/local/lib/python3.7/dist-packages (from datasets) (6.0.1)\n",
            "Requirement already satisfied: numpy>=1.17 in /usr/local/lib/python3.7/dist-packages (from datasets) (1.21.6)\n",
            "Requirement already satisfied: importlib-metadata in /usr/local/lib/python3.7/dist-packages (from datasets) (5.0.0)\n",
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          ]
        }
      ]
    },
    {
      "cell_type": "code",
      "source": [
        "!python3 -m pip install rouge_score"
      ],
      "metadata": {
        "colab": {
          "base_uri": "https://localhost:8080/"
        },
        "id": "Io56QEJ9RkZK",
        "outputId": "22911231-f26c-4347-e2e4-727b245148b6"
      },
      "execution_count": null,
      "outputs": [
        {
          "output_type": "stream",
          "name": "stdout",
          "text": [
            "Looking in indexes: https://pypi.org/simple, https://us-python.pkg.dev/colab-wheels/public/simple/\n",
            "Collecting rouge_score\n",
            "  Downloading rouge_score-0.1.2.tar.gz (17 kB)\n",
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            "Building wheels for collected packages: rouge-score\n",
            "  Building wheel for rouge-score (setup.py) ... \u001b[?25l\u001b[?25hdone\n",
            "  Created wheel for rouge-score: filename=rouge_score-0.1.2-py3-none-any.whl size=24955 sha256=74e9f1b29d1c30d1dadfcdba858d72d2db4598e996bb9a235ee4ca87d2030f18\n",
            "  Stored in directory: /root/.cache/pip/wheels/84/ac/6b/38096e3c5bf1dc87911e3585875e21a3ac610348e740409c76\n",
            "Successfully built rouge-score\n",
            "Installing collected packages: rouge-score\n",
            "Successfully installed rouge-score-0.1.2\n"
          ]
        }
      ]
    },
    {
      "cell_type": "code",
      "source": [
        "from datasets import load_dataset_builder, load_dataset\n",
        "from datasets import get_dataset_config_names\n",
        "\n",
        "from tqdm.auto import tqdm  # for our loading bar\n",
        "from sumy.parsers.plaintext import PlaintextParser\n",
        "from sumy.nlp.tokenizers import Tokenizer\n",
        "from sumy.summarizers.lex_rank import LexRankSummarizer\n",
        "import pandas as pd\n",
        "import nltk\n",
        "nltk.download('punkt')\n",
        "\n",
        "from google.colab import drive\n",
        "drive.mount('drive')\n",
        "\n",
        "def get_num_words(sentence):\n",
        "  print(len(sentence.split()))\n",
        "  return len(sentence.split())\n"
      ],
      "metadata": {
        "colab": {
          "base_uri": "https://localhost:8080/"
        },
        "id": "Oz-fPWTH2t6p",
        "outputId": "d9ad9953-ea90-49c2-bcb9-1403a7034cac"
      },
      "execution_count": null,
      "outputs": [
        {
          "output_type": "stream",
          "name": "stderr",
          "text": [
            "[nltk_data] Downloading package punkt to /root/nltk_data...\n",
            "[nltk_data]   Unzipping tokenizers/punkt.zip.\n"
          ]
        },
        {
          "output_type": "stream",
          "name": "stdout",
          "text": [
            "Mounted at drive\n"
          ]
        }
      ]
    },
    {
      "cell_type": "code",
      "source": [
        "# PUBMED\n",
        "configs = get_dataset_config_names(\"ccdv/pubmed-summarization\")\n",
        "print(configs)\n",
        "\n",
        "ds_builder = load_dataset_builder(\"ccdv/pubmed-summarization\", \"document\")\n",
        "print(ds_builder.info.description)\n",
        "print(ds_builder.info.features)\n",
        "\n",
        "dataset = load_dataset(\"ccdv/pubmed-summarization\")\n",
        "print(dataset)\n",
        "print(dataset['train'][1])\n",
        "\n",
        "small_train_dataset = dataset[\"train\"].shuffle(seed=42).select(range(1000))\n",
        "small_eval_dataset = dataset[\"validation\"].shuffle(seed=42).select(range(100))\n",
        "\n"
      ],
      "metadata": {
        "colab": {
          "base_uri": "https://localhost:8080/",
          "height": 661,
          "referenced_widgets": [
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        },
        "id": "5lXHbERgYiMu",
        "outputId": "88868369-ffb2-472f-8c5d-9e3d87d0cf39"
      },
      "execution_count": null,
      "outputs": [
        {
          "output_type": "display_data",
          "data": {
            "text/plain": [
              "Downloading builder script:   0%|          | 0.00/5.13k [00:00<?, ?B/s]"
            ],
            "application/vnd.jupyter.widget-view+json": {
              "version_major": 2,
              "version_minor": 0,
              "model_id": "3926fa3b7e38408eb6b3d3946f654691"
            }
          },
          "metadata": {}
        },
        {
          "output_type": "stream",
          "name": "stdout",
          "text": [
            "['section', 'document']\n",
            "\n",
            " PubMed dataset for summarization.\n",
            " From paper: A Discourse-Aware Attention Model for Abstractive Summarization of Long Documents\" by A. Cohan et al.\n",
            " See: https://aclanthology.org/N18-2097.pdf \n",
            " See: https://github.com/armancohan/long-summarization\n",
            "\n",
            "{'article': Value(dtype='string', id=None), 'abstract': Value(dtype='string', id=None)}\n"
          ]
        },
        {
          "output_type": "stream",
          "name": "stderr",
          "text": [
            "WARNING:datasets.builder:No config specified, defaulting to: pubmed-summarization/section\n"
          ]
        },
        {
          "output_type": "stream",
          "name": "stdout",
          "text": [
            "Downloading and preparing dataset pubmed-summarization/section to /root/.cache/huggingface/datasets/ccdv___pubmed-summarization/section/1.0.0/f765ec606c790e8c5694b226814a13f1974ba4ea98280989edaffb152ded5e2b...\n"
          ]
        },
        {
          "output_type": "display_data",
          "data": {
            "text/plain": [
              "Downloading data:   0%|          | 0.00/779M [00:00<?, ?B/s]"
            ],
            "application/vnd.jupyter.widget-view+json": {
              "version_major": 2,
              "version_minor": 0,
              "model_id": "851c4305db9b468aa2eb7ab396ba566b"
            }
          },
          "metadata": {}
        },
        {
          "output_type": "display_data",
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            ],
            "application/vnd.jupyter.widget-view+json": {
              "version_major": 2,
              "version_minor": 0,
              "model_id": "a59c551a425444489ec9d3c9d1cc68f7"
            }
          },
          "metadata": {}
        },
        {
          "output_type": "display_data",
          "data": {
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              "Downloading data:   0%|          | 0.00/43.8M [00:00<?, ?B/s]"
            ],
            "application/vnd.jupyter.widget-view+json": {
              "version_major": 2,
              "version_minor": 0,
              "model_id": "da9afeec29f944559c9c74a29018d7fb"
            }
          },
          "metadata": {}
        },
        {
          "output_type": "display_data",
          "data": {
            "text/plain": [
              "Generating train split: 0 examples [00:00, ? examples/s]"
            ],
            "application/vnd.jupyter.widget-view+json": {
              "version_major": 2,
              "version_minor": 0,
              "model_id": "25a76a0135b04ff58e26ec420c06a16d"
            }
          },
          "metadata": {}
        },
        {
          "output_type": "display_data",
          "data": {
            "text/plain": [
              "Generating validation split: 0 examples [00:00, ? examples/s]"
            ],
            "application/vnd.jupyter.widget-view+json": {
              "version_major": 2,
              "version_minor": 0,
              "model_id": "80bcc2de7b7346da86f67c60706db0eb"
            }
          },
          "metadata": {}
        },
        {
          "output_type": "display_data",
          "data": {
            "text/plain": [
              "Generating test split: 0 examples [00:00, ? examples/s]"
            ],
            "application/vnd.jupyter.widget-view+json": {
              "version_major": 2,
              "version_minor": 0,
              "model_id": "71a59054ac544fa18debbd721c1b45b8"
            }
          },
          "metadata": {}
        },
        {
          "output_type": "stream",
          "name": "stdout",
          "text": [
            "Dataset pubmed-summarization downloaded and prepared to /root/.cache/huggingface/datasets/ccdv___pubmed-summarization/section/1.0.0/f765ec606c790e8c5694b226814a13f1974ba4ea98280989edaffb152ded5e2b. Subsequent calls will reuse this data.\n"
          ]
        },
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            }
          },
          "metadata": {}
        },
        {
          "output_type": "stream",
          "name": "stdout",
          "text": [
            "DatasetDict({\n",
            "    train: Dataset({\n",
            "        features: ['article', 'abstract'],\n",
            "        num_rows: 119924\n",
            "    })\n",
            "    validation: Dataset({\n",
            "        features: ['article', 'abstract'],\n",
            "        num_rows: 6633\n",
            "    })\n",
            "    test: Dataset({\n",
            "        features: ['article', 'abstract'],\n",
            "        num_rows: 6658\n",
            "    })\n",
            "})\n",
            "{'article': 'it occurs in more than 50% of patients and may reach 90% in certain types of cancers , especially in patients undergoing chemotherapy and/or radiation therapy.1 anemia is defined as an inadequate circulating level of hemoglobin ( hb ) ( hb < 12 g / dl ) and may arise as a result of the underlying disease , bleeding , poor nutrition , chemotherapy , or radiation therapy . \\n preliminary studies suggest that survival and loco - regional control after radiation therapy , especially in head and neck cancers , may be compromised by anemia.24 anemia often worsens symptoms such as fatigue , weakness , and dyspnea , and thus may have a negative effect on quality of life ( qol ) and performance status in patients with cancer . \\n thus , to improve physical functioning , qol , and prognosis in patients with cancer , it would be reasonable to take a proactive approach in identifying populations who need treatment for cancer - associated anemia ( caa ) and provide timely management . \\n blood transfusion is an effective way to replace depleted hb within a short period , but the effect is , unfortunately , temporary and can cause serious adverse risks and increased mortality . in randomized clinical trials in patients with caa \\n , erythropoiesis - stimulating agents ( esas ) produced significant increases in hb level , decreased transfusion requirements , and improved qol.57 however , 30%50% of patients do not respond to such agents . \\n in addition , the use of esas often causes concern about severe adverse reactions.6,8 in several studies , esas were found to shorten overall survival time , or time to tumor progression in patients whose hb level reached more than 12 g / dl . \\n these studies included patients with different primary cancers , such as breast , lung , head and neck , cervix , and lymphomas.911 the lack of response to erythropoietin stimulation in patients with cancer is partly attributed to the functional iron deficiency state , in which the high rate of erythropoiesis exceeds the delivery of usable iron , despite adequate iron stores.12 absolute iron deficiency , in contrast , occurs when iron delivery is impaired because iron stores are depleted ( serum ferritin , < 100 ng / ml ; transferring saturation , < 20%).13 hepcidin , a peptide hormone produced by the liver , is up - regulated in chronic inflammatory states including cancer . \\n hepcidin inhibits iron transport across cell membranes , thus decreasing the accessibility of stored iron and gastrointestinal absorption of dietary iron , leading to an increased frequency of iron - restricted erythropoiesis.1416 many randomized trials examined the role of intravenous ( iv ) iron in addition to esas in the treatment of anemia in patients with cancer . \\n many of these studies showed improvement in esa response , time to maximal response , reduction in esa dose , and improvement in qol parameters ( when measured ) in favor of the combination over esas alone . \\n the observed benefit was independent of baseline iron parameters.1721 one study found a 36% reduction in the number of patients transfused.21 this pilot study assessed the efficacy and feasibility of iv iron monotherapy in patients with cancer who have anemia and who are undergoing treatment with chemotherapy and/or radiation therapy without the use of esas . \\n patients received the study treatment for 12 weeks followed by a 4-week follow - up period . \\n eligible patients were at least 18 years old , about to start a cycle of chemotherapy and/or radiation therapy within 1 week of inclusion , and had a nonmyeloid malignancy , hb levels of 11.0 g / dl or less , a life expectancy of more than 24 weeks , and an eastern cooperative oncology group performance status of 02 . \\n patients were also required to have a serum ferritin level of 100 ng / ml or higher or transferrin saturation ( tsat ) levels of 15% or higher and to have received no esas or iv iron therapy within 30 days and no oral iron therapy ( 27 mg / day or more ) within 7 days before enrollment . \\n patients were excluded for leukoerythroblastic features on blood film , hemolysis , gastrointestinal bleeding , folate or vitamin b12 deficiency , elevated serum ferritin ( 900 ng / ml ) or transferrin saturation ( tsat ) ( 35% ) levels , pregnancy or lactation , liver dysfunction ( grade 2 or higher based on national cancer institute common toxicity criteria ) , renal dysfunction ( serum creatinine levels 2.0 mg / dl ) , active infection requiring systemic antibiotics , personal or family history of hemochromatosis , comorbidities precluding study participation , hypersensitivity to iv iron , red blood cell transfusion within the last 2 weeks , or any investigational agent within 30 days before enrollment . \\n patients were not allowed to take any vitamin , mineral , or herbal supplements containing 27 mg or more of iron per day or 100 mg vitamin c per day during the study or follow - up period . \\n blood transfusions were permitted at the primary physician s discretion if hb levels decreased to 8 g / dl or less , and such patients were considered treatment failures . \\n written informed consent was provided by all patients before study participation , and the protocol and supporting documents were approved by the institutional review board of king hussein cancer center . \\n the study was conducted in accordance with the declaration of helsinki and good clinical practice as contained in the us code of federal regulations that governs the protection of human subjects and the obligations of clinical investigators . \\n patients received 200 mg ferric hydroxide sucrose diluted in 100 ml normal saline and infused over the course of 1 hour weekly for a total of 12 weeks . the first dose was given during the first clinic visit ( 4 days from the initiation of chemotherapy or radiation therapy ) . \\n tsat was monitored , as protocol mandated withholding iron therapy when tsat levels were higher than 50% . at the first clinic visit ( week 1 ; baseline ) , a blood sample was obtained for laboratory assessments before the study treatment was started . \\n patients attended weekly clinic visits for treatment and assessment ; and returned for follow - up visits at week 14 which included a complete physical examination . \\n complete blood count and tsat were done every 3 weeks , and again 2 weeks after last treatment ( week 14 ) . \\n complete laboratory assessment ( hb , serum ferritin , reticulocyte count , transferrin , tsat , serum iron , total iron binding capacity , red cell indices , white blood cell count with differential , platelet count , and serum chemistries ) were done at week 1 and at week 14 ( end of study ) . \\n adverse events were assessed at each clinic visit until study completion or withdrawal , and during the 30 days after the last study treatment . \\n hb test results were presented as mean , median , and range through all 12 weeks . \\n comparison between means of hb level were made between the baseline hb and hb levels in the following weeks , using t - test . a significance criterion of p < 0.05 was used in the analysis . \\n all analyses were performed using sas version 9.1 ( sas institute inc , cary , nc , usa ) . \\n patients received the study treatment for 12 weeks followed by a 4-week follow - up period . \\n eligible patients were at least 18 years old , about to start a cycle of chemotherapy and/or radiation therapy within 1 week of inclusion , and had a nonmyeloid malignancy , hb levels of 11.0 g / dl or less , a life expectancy of more than 24 weeks , and an eastern cooperative oncology group performance status of 02 . \\n patients were also required to have a serum ferritin level of 100 ng / ml or higher or transferrin saturation ( tsat ) levels of 15% or higher and to have received no esas or iv iron therapy within 30 days and no oral iron therapy ( 27 mg / day or more ) within 7 days before enrollment . \\n patients were excluded for leukoerythroblastic features on blood film , hemolysis , gastrointestinal bleeding , folate or vitamin b12 deficiency , elevated serum ferritin ( 900 ng / ml ) or transferrin saturation ( tsat ) ( 35% ) levels , pregnancy or lactation , liver dysfunction ( grade 2 or higher based on national cancer institute common toxicity criteria ) , renal dysfunction ( serum creatinine levels 2.0 mg / dl ) , active infection requiring systemic antibiotics , personal or family history of hemochromatosis , comorbidities precluding study participation , hypersensitivity to iv iron , red blood cell transfusion within the last 2 weeks , or any investigational agent within 30 days before enrollment . \\n patients were not allowed to take any vitamin , mineral , or herbal supplements containing 27 mg or more of iron per day or 100 mg vitamin c per day during the study or follow - up period . \\n blood transfusions were permitted at the primary physician s discretion if hb levels decreased to 8 g / dl or less , and such patients were considered treatment failures . \\n written informed consent was provided by all patients before study participation , and the protocol and supporting documents were approved by the institutional review board of king hussein cancer center . \\n the study was conducted in accordance with the declaration of helsinki and good clinical practice as contained in the us code of federal regulations that governs the protection of human subjects and the obligations of clinical investigators . \\n patients received 200 mg ferric hydroxide sucrose diluted in 100 ml normal saline and infused over the course of 1 hour weekly for a total of 12 weeks . \\n the first dose was given during the first clinic visit ( 4 days from the initiation of chemotherapy or radiation therapy ) . \\n tsat was monitored , as protocol mandated withholding iron therapy when tsat levels were higher than 50% . \\n at the first clinic visit ( week 1 ; baseline ) , a blood sample was obtained for laboratory assessments before the study treatment was started . \\n patients attended weekly clinic visits for treatment and assessment ; and returned for follow - up visits at week 14 which included a complete physical examination . \\n complete blood count and tsat were done every 3 weeks , and again 2 weeks after last treatment ( week 14 ) . \\n complete laboratory assessment ( hb , serum ferritin , reticulocyte count , transferrin , tsat , serum iron , total iron binding capacity , red cell indices , white blood cell count with differential , platelet count , and serum chemistries ) were done at week 1 and at week 14 ( end of study ) . \\n adverse events were assessed at each clinic visit until study completion or withdrawal , and during the 30 days after the last study treatment . \\n hb test results were presented as mean , median , and range through all 12 weeks . \\n comparison between means of hb level were made between the baseline hb and hb levels in the following weeks , using t - test . a significance criterion of p < 0.05 was used in the analysis . \\n all analyses were performed using sas version 9.1 ( sas institute inc , cary , nc , usa ) . \\n twenty - five patients ( 17 women and 8 men ) were eligible , consented , and included in the study ; their mean age ( standard deviation , [ sd ] ) was 56 years ( 13.0 years ) . \\n chemotherapy varied according to the primary cancer and included anthracycline , platinum , taxanes , cyclophosphamide , high - dose ifosfamide , vincristine , vinblastine , bleomycin , and others . \\n many of the included patients had their chemotherapy treatment as second- or third - line therapy . \\n patients characteristics , including age , primary tumor , and active anticancer treatment are summarized in table 1 . \\n one patient died during the study from his tumor ( after week 2 ) , and five patients withdrew from the study because of inconvenience ( three after week 3 , and two after week 4 ) . \\n nineteen ( 76.0% ) patients completed a minimum of three treatments , 15 ( 60.0% ) completed nine treatments , and 14 ( 56.0% ) completed all twelve planned weekly treatments . \\n as seen in table 2 , the mean hb level of the 25 patients at baseline was 9.6 g / dl ( median , 9.9 g / dl ; range , 6.9 g / dl10.9 g / dl ) . for the 15 patients who completed at least nine treatments , the mean change in their hb level was 1.7 g / dl ( median , 1.1 g / dl ; range , 1.9 g / dl to 3.2 g / dl ) . \\n for the 14 patients who completed the whole treatment period ( 12 weeks ) , the mean hb level change was 2.1 g / dl ( median , 1.3 g / dl ; range , 0.2 g / dl to 4.6 g / dl ; p = 0.0007 ) . \\n eight ( 42.1% ) of the 19 patients who completed at least three iron infusions had a more than 1 g / dl increase in their hb level . \\n hemoglobin level changes for the 14 patients who completed twelve iron infusions are shown in figure 1 . \\n no iv iron - related adverse events were reported among patients during the study or the follow - up period . \\n tsat was monitored during the study period , and no patients had tsat levels increase to more than 50% . \\n the highest ferritin level among patients who completed at least nine iv iron treatments was 1,170 ng / ml ; the mean level at the end of study period for the whole group was 379 ng / ml . \\n five ( 20.0% ) patients received blood transfusions and were considered treatment failures ( three after week 3 , transfused at hb levels of 6.9 g / dl , 7.8 g / dl , and 5.4 g / dl ; one after week 4 , transfused at an hb level of 8.2 g / dl ; and one after week 9 , transfused at an hb level of 7.2 g / dl ) . \\n low hb levels are associated with diminished qol and possibly decreased overall survival.2 successful treatment of anemia has undeniable benefits for patients , often yielding dramatic symptomatic improvement . \\n although the role of esas is well - established in treating caa , big concerns were recently raised about the negative effect of esas on survival in some patients with cancer.911 concerns about the risk for thromboembolism in patients with cancer with higher hb levels who are receiving esa were also addressed in many trials.22,23 in addition , the possible immunosuppressive effects of blood product transfusions that may have relevance to neoplasia progression were addressed before.24 , 25 in our pilot study , we tested the feasibility of using iron supplementation alone to treat anemia in patients with cancer who are undergoing chemotherapy without the use of esas or blood transfusion , which could be a valid alternative , especially for patients with curable cancers . \\n oral iron is easier to administer and relatively inexpensive , but low patient adherence , poor enteral absorption , and poor tolerance because of a wide range of troublesome gastrointestinal adverse effects limit its overall effectiveness.26 anemia of chronic disease may occur in patients with cancer and is associated with an increase in hepcidin levels , which decreases oral iron absorption and bone marrow iron use , negating any possible effect of regular doses of oral iron.15 iv iron therapy significantly improves response to epoetin alfa when compared with oral iron or no iron in anemic patients with cancer who are receiving chemotherapy.1721 oral iron supplements with esas showed no significant benefit over esas alone in treating caa.21 sodium ferric gluconate and iron sucrose appear to have more favorable safety profiles over iron dextran . \\n a large prospective safety comparison trial failed to show serious anaphylactoid reactions,27 which is confirmed in our study , in which no patients developed reactions and no patients withdrew from the study because of adverse effects . given that the mean hb increase using esas with iv iron in one large controlled trial was 2.4 g / dl,21 the results obtained in our study are clinically significant . \\n these findings should be further confirmed and better assessed in larger studies , in which questions such as the optimal timing of iv iron therapy with respect to chemotherapy and the optimal total dose of iv iron should be determined . \\n the use of iv iron monotherapy was recently reviewed by a group in germany that studied the use of ferric carboxymaltose to replace esa and blood transfusions as a treatment for caa . \\n iron - deficient patients treated with ferric carboxymaltose alone ( n = 233 ) had a median of 1.4 g / dl increase in hemoglobin levels compared with those receiving additional treatment with esas ( n = 46 ; median , 1.6 g / dl ) . our study , \\n however , is peculiar in using iron therapy in a non - iron - deficiency state.28 iron overload after iv iron therapy , with potential concerns about the risk of developing secondary cancers and infection , might be raised . \\n the highest serum ferritin level in the present study in patients who completed at least 9 weeks of iv iron therapy was 1,170 ng / ml . most of the literature addressing cancer and infections in iron - overloaded patients comes from patients with hemochromatosis or patients who are undergoing hemodialysis . \\n published reviews report an increase in hepatocellular carcinoma only in patients with hemochromatosis after they develop cirrhosis.29 similarly data supporting the association between iv iron therapy and higher infection rate are weak and not well - supported.30 in fact , anemia itself is a risk factor for infections in patients receiving hemodialysis.31 a multivariate analysis of associations between iron and mortality in more than 58,000 patients receiving hemodialysis reported no increased death rate from serum ferritin levels as high as 1,200 ng / ml.30 the increasing cost of therapy in patients with cancer is of grave concern , which could be an additional benefit of iv iron over the use of esas in such patients . to further address many of the questions raised , \\n our team is planning a bigger trial for iv iron in patients with cancer who have anemia to confirm the results discussed in this pilot trial . \\n in addition , we will be looking into predictors of response to iv iron , such as serum hepcidin level . \\n iv iron therapy alone is safe and may be effective in improving hb levels in patients with cancer who are undergoing active anticancer therapy . \\n further randomized trials are needed to address many of the questions raised in our pilot study .', 'abstract': 'backgroundanemia in patients with cancer who are undergoing active therapy is commonly encountered and may worsen quality of life in these patients . the effect of blood transfusion is often temporary and may be associated with serious adverse events . \\n erythropoiesis - stimulating agents are not effective in 30%50% of patients and may have a negative effect on overall survival.aimsto assess the efficacy and feasibility of intravenous iron therapy in patients with cancer who have non - iron - deficiency anemia and who are undergoing treatment with chemotherapy without the use of erythropoiesis - stimulating agents.methodsadult patients with solid cancers and non - iron - deficiency anemia were included . \\n ferric sucrose at a dose of 200 mg was given in short intravenous infusions weekly for a total of 12 weeks . \\n hemoglobin level was measured at baseline , every 3 weeks , and 2 weeks after the last iron infusion ( week 14 ) . \\n adverse events related to intravenous iron were prospectively reported.resultsof 25 patients included , 19 ( 76.0% ) completed at least three iron infusions and 14 ( 56.0% ) finished the planned 12 weeks of therapy . \\n the mean hemoglobin level of the 25 patients at baseline was 9.6 g / dl ( median , 9.9 g / dl ; range , 6.9 g / dl 10.9 g / dl ) . the mean change in hemoglobin level for the 15 patients who completed at least 9 treatments was 1.7 g / dl ( median , 1.1 g / dl ; range , 1.9 g / dl to 3.2 g / dl ) ; it reached 2.1 g / dl ( median , 1.3 g / dl ; range , 0.2 g / dl to 4.6 g / dl ; p = 0.0007 ) for the 14 patients who completed all 12 weekly treatments . \\n five ( 20.0% ) patients were transfused and considered as treatment failures . \\n no treatment - related adverse events were reported.conclusionintravenous iron treatment alone is safe and may reduce blood transfusion requirements and improve hemoglobin level in patients with cancer who are undergoing anticancer therapy . \\n further randomized studies are needed to confirm these findings .'}\n"
          ]
        }
      ]
    },
    {
      "cell_type": "code",
      "source": [
        "# ARXIV\n",
        "configs = get_dataset_config_names(\"ccdv/arxiv-summarization\")\n",
        "print(configs)\n",
        "\n",
        "ds_builder = load_dataset_builder(\"ccdv/arxiv-summarization\", \"document\")\n",
        "print(ds_builder.info.description)\n",
        "print(ds_builder.info.features)\n",
        "\n",
        "dataset = load_dataset(\"ccdv/arxiv-summarization\")\n",
        "print(dataset)\n",
        "print(dataset['train'][1])\n",
        "\n",
        "small_train_dataset = dataset[\"train\"].shuffle(seed=42).select(range(1000))\n",
        "small_eval_dataset = dataset[\"validation\"].shuffle(seed=42).select(range(100))\n",
        "\n"
      ],
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        },
        "outputId": "470533c2-05ed-4d9e-bf36-a137693f3d8d"
      },
      "execution_count": null,
      "outputs": [
        {
          "output_type": "display_data",
          "data": {
            "text/plain": [
              "Downloading builder script:   0%|          | 0.00/5.14k [00:00<?, ?B/s]"
            ],
            "application/vnd.jupyter.widget-view+json": {
              "version_major": 2,
              "version_minor": 0,
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          "metadata": {}
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        {
          "output_type": "stream",
          "name": "stdout",
          "text": [
            "['section', 'document']\n",
            "\n",
            " Arxiv dataset for summarization.\n",
            " From paper: A Discourse-Aware Attention Model for Abstractive Summarization of Long Documents\" by A. Cohan et al.\n",
            " See: https://aclanthology.org/N18-2097.pdf \n",
            " See: https://github.com/armancohan/long-summarization\n",
            "\n",
            "{'article': Value(dtype='string', id=None), 'abstract': Value(dtype='string', id=None)}\n"
          ]
        },
        {
          "output_type": "stream",
          "name": "stderr",
          "text": [
            "WARNING:datasets.builder:No config specified, defaulting to: arxiv-summarization/section\n"
          ]
        },
        {
          "output_type": "stream",
          "name": "stdout",
          "text": [
            "Downloading and preparing dataset arxiv-summarization/section to /root/.cache/huggingface/datasets/ccdv___arxiv-summarization/section/1.0.0/fa2c9abf4312afb8660ef8e041d576b8e3943ea96ae771bd3cd091b5798e7cc3...\n"
          ]
        },
        {
          "output_type": "display_data",
          "data": {
            "text/plain": [
              "Downloading data:   0%|          | 0.00/3.36G [00:00<?, ?B/s]"
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          "output_type": "display_data",
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              "Downloading data:   0%|          | 0.00/102M [00:00<?, ?B/s]"
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              "Downloading data:   0%|          | 0.00/102M [00:00<?, ?B/s]"
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        {
          "output_type": "display_data",
          "data": {
            "text/plain": [
              "Generating train split: 0 examples [00:00, ? examples/s]"
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            "application/vnd.jupyter.widget-view+json": {
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              "model_id": "53f36c23624b4c7ba26ce940181b483a"
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          "metadata": {}
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        {
          "output_type": "display_data",
          "data": {
            "text/plain": [
              "Generating validation split: 0 examples [00:00, ? examples/s]"
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        {
          "output_type": "display_data",
          "data": {
            "text/plain": [
              "Generating test split: 0 examples [00:00, ? examples/s]"
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              "model_id": "88878100dd6b45058ce0e7b454164add"
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          "output_type": "stream",
          "name": "stdout",
          "text": [
            "Dataset arxiv-summarization downloaded and prepared to /root/.cache/huggingface/datasets/ccdv___arxiv-summarization/section/1.0.0/fa2c9abf4312afb8660ef8e041d576b8e3943ea96ae771bd3cd091b5798e7cc3. Subsequent calls will reuse this data.\n"
          ]
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        {
          "output_type": "display_data",
          "data": {
            "text/plain": [
              "  0%|          | 0/3 [00:00<?, ?it/s]"
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          "text": [
            "DatasetDict({\n",
            "    train: Dataset({\n",
            "        features: ['article', 'abstract'],\n",
            "        num_rows: 203037\n",
            "    })\n",
            "    validation: Dataset({\n",
            "        features: ['article', 'abstract'],\n",
            "        num_rows: 6436\n",
            "    })\n",
            "    test: Dataset({\n",
            "        features: ['article', 'abstract'],\n",
            "        num_rows: 6440\n",
            "    })\n",
            "})\n",
            "{'article': 'the leptonic decays of a charged pseudoscalar meson @xmath7 are processes of the type @xmath8 , where @xmath9 , @xmath10 , or @xmath11 . because no strong interactions are present in the leptonic final state @xmath12 , such decays provide a clean way to probe the complex , strong interactions that bind the quark and antiquark within the initial - state meson . in these decays , strong interaction effects can be parametrized by a single quantity , @xmath13 , the pseudoscalar meson decay constant . \\n the leptonic decay rate can be measured by experiment , and the decay constant can be determined by the equation ( ignoring radiative corrections ) @xmath14 where @xmath15 is the fermi coupling constant , @xmath16 is the cabibbo - kobayashi - maskawa ( ckm ) matrix  @xcite element , @xmath17 is the mass of the meson , and @xmath18 is the mass of the charged lepton . \\n the quantity @xmath13 describes the amplitude for the @xmath19 and @xmath20-quarks within the @xmath21 to have zero separation , a condition necessary for them to annihilate into the virtual @xmath22 boson that produces the @xmath12 pair . \\n the experimental determination of decay constants is one of the most important tests of calculations involving nonperturbative qcd . \\n such calculations have been performed using various models  @xcite or using lattice qcd ( lqcd ) . \\n the latter is now generally considered to be the most reliable way to calculate the quantity . \\n knowledge of decay constants is important for describing several key processes , such as @xmath23 mixing , which depends on @xmath24 , a quantity that is also predicted by lqcd calculations . \\n experimental determination  @xcite of @xmath24 with the leptonic decay of a @xmath25 meson is , however , very limited as the rate is highly suppressed due to the smallness of the magnitude of the relevant ckm matrix element @xmath26 . \\n the charm mesons , @xmath27 and @xmath28 , are better instruments to study the leptonic decays of heavy mesons since these decays are either less ckm suppressed or favored , _ \\n i.e. _ , @xmath29 and @xmath30 are much larger than @xmath31 . \\n thus , the decay constants @xmath32 and @xmath33 determined from charm meson decays can be used to test and validate the necessary lqcd calculations applicable to the @xmath34-meson sector .    among \\n the leptonic decays in the charm - quark sector , @xmath35 decays are more accessible since they are ckm favored . \\n furthermore , the large mass of the @xmath11 lepton removes the helicity suppression that is present in the decays to lighter leptons . \\n the existence of multiple neutrinos in the final state , however , makes measurement of this decay challenging . \\n physics beyond the standard model ( sm ) might also affect leptonic decays of charmed mesons . \\n depending on the non - sm features , the ratio of @xmath36 could be affected  @xcite , as could the ratio  @xcite @xmath37 . \\n any of the individual widths might be increased or decreased . \\n there is an indication of a discrepancy between the experimental determinations  @xcite of @xmath33 and the most recent precision lqcd calculation  @xcite . \\n this disagreement is particularly puzzling since the cleo - c determination  @xcite of @xmath32 agrees well with the lqcd calculation  @xcite of that quantity . some  @xcite conjecture that this discrepancy may be explained by a charged higgs boson or a leptoquark .    in this article \\n , we report an improved measurement of the absolute branching fraction of the leptonic decay @xmath0 ( charge - conjugate modes are implied ) , with @xmath1 , from which we determine the decay constant @xmath33 . \\n we use a data sample of @xmath38 events provided by the cornell electron storage ring ( cesr ) and collected by the cleo - c detector at the center - of - mass ( cm ) energy @xmath39 mev , near @xmath3 peak production  @xcite . \\n the data sample consists of an integrated luminosity of @xmath40 @xmath41 containing @xmath42 @xmath3 pairs . \\n we have previously reported  @xcite measurements of @xmath43 and @xmath0 with a subsample of these data . a companion article  @xcite reports measurements of @xmath33 from @xmath43 and @xmath0 , with @xmath44 , using essentially the same data sample as the one used in this measurement . \\n the cleo - c detector  @xcite is a general - purpose solenoidal detector with four concentric components utilized in this measurement : a small - radius six - layer stereo wire drift chamber , a 47-layer main drift chamber , a ring - imaging cherenkov ( rich ) detector , and an electromagnetic calorimeter consisting of 7800 csi(tl ) crystals . \\n the two drift chambers operate in a @xmath45  t magnetic field and provide charged particle tracking in a solid angle of @xmath46% of @xmath47 . \\n the chambers achieve a momentum resolution of @xmath48% at @xmath49  gev/@xmath50 . \\n the main drift chamber also provides specific - ionization ( @xmath51 ) measurements that discriminate between charged pions and kaons . \\n the rich detector covers approximately @xmath52% of @xmath47 and provides additional separation of pions and kaons at high momentum . \\n the photon energy resolution of the calorimeter is @xmath53% at @xmath54  gev and @xmath55% at @xmath56  mev . \\n electron identification is based on a likelihood variable that combines the information from the rich detector , @xmath51 , and the ratio of electromagnetic shower energy to track momentum ( @xmath57 ) . \\n we use a geant - based  @xcite monte carlo ( mc ) simulation program to study efficiency of signal - event selection and background processes . \\n physics events are generated by evtgen  @xcite , tuned with much improved knowledge of charm decays  @xcite , and final - state radiation ( fsr ) is modeled by the photos  @xcite program . \\n the modeling of initial - state radiation ( isr ) is based on cross sections for @xmath3 production at lower energies obtained from the cleo - c energy scan  @xcite near the cm energy where we collect the sample . \\n the presence of two @xmath58 mesons in a @xmath3 event allows us to define a single - tag ( st ) sample in which a @xmath58 is reconstructed in a hadronic decay mode and a further double - tagged ( dt ) subsample in which an additional @xmath59 is required as a signature of @xmath60 decay , the @xmath59 being the daughter of the @xmath60 . \\n the @xmath61 reconstructed in the st sample can be either primary or secondary from @xmath62 ( or @xmath63 ) . \\n the st yield can be expressed as @xmath64 where @xmath65 is the produced number of @xmath3 pairs , @xmath66 is the branching fraction of hadronic modes used in the st sample , and @xmath67 is the st efficiency . \\n the @xmath68 counts the candidates , not events , and the factor of 2 comes from the sum of @xmath28 and @xmath61 tags . \\n our double - tag ( dt ) sample is formed from events with only a single charged track , identified as an @xmath69 , in addition to a st . \\n the yield can be expressed as @xmath70 where @xmath71 is the leptonic decay branching fraction , including the subbranching fraction of @xmath1 decay , @xmath72 is the efficiency of finding the st and the leptonic decay in the same event . from the st and dt yields we can obtain an absolute branching fraction of the leptonic decay @xmath71 , without needing to know the integrated luminosity or the produced number of @xmath3 pairs , @xmath73 where @xmath74 ( @xmath75 ) is the effective signal efficiency . because of the large solid angle acceptance with high segmentation of the cleo - c detector and the low multiplicity of the events with which we are concerned , @xmath76 , where @xmath77 is the leptonic decay efficiency . \\n hence , the ratio @xmath78 is insensitive to most systematic effects associated with the st , and the signal branching fraction @xmath71 obtained using this procedure is nearly independent of the efficiency of the tagging mode .      to minimize systematic uncertainties , we tag using three two - body hadronic decay modes with only charged particles in the final state . \\n the three st modes and @xmath79 are shorthand labels for @xmath80 events within mass windows ( described below ) of the @xmath81 peak in @xmath82 and the @xmath83 peak in @xmath84 , respectively . \\n no attempt is made to separate these resonance components in the @xmath85 dalitz plot . ] \\n are @xmath86 , @xmath79 , and @xmath87 . \\n using these tag modes also helps to reduce the tag bias which would be caused by the correlation between the tag side and the signal side reconstruction if tag modes with high multiplicity and large background were used . \\n the effect of the tag bias @xmath88 can be expressed in terms of the signal efficiency @xmath74 defined by @xmath89 where @xmath90 is the st efficiency when the recoiling system is the signal leptonic decay with single @xmath59 in the other side of the tag . \\n as the general st efficiency @xmath67 , when the recoiling system is any possible @xmath91 decays , will be lower than the @xmath90 , sizable tag bias could be introduced if the multiplicity of the tag mode were high , or the tag mode were to include neutral particles in the final state . as shown in sec . \\n [ sec : results ] , this effect is negligible in our chosen clean tag modes . \\n the @xmath92 decay is reconstructed by combining oppositely charged tracks that originate from a common vertex and that have an invariant mass within @xmath93 mev of the nominal mass  @xcite . \\n we require the resonance decay to satisfy the following mass windows around the nominal masses  @xcite : @xmath94 ( @xmath95 mev ) and @xmath96 ( @xmath97 mev ) . \\n we require the momenta of charged particles to be @xmath56 mev or greater to suppress the slow pion background from @xmath98 decays ( through @xmath99 ) . \\n we identify a st by using the invariant mass of the tag @xmath100 and recoil mass against the tag @xmath101 . \\n the recoil mass is defined as @xmath102 where @xmath103 is the net four - momentum of the @xmath4 beam , taking the finite beam crossing angle into account ; @xmath104 is the four - momentum of the tag , with @xmath105 computed from @xmath106 and the nominal mass  @xcite of the @xmath91 meson . \\n we require the recoil mass to be within @xmath107 mev of the @xmath108 mass  @xcite . \\n this loose window allows both primary and secondary @xmath91 tags to be selected .        to estimate the backgrounds in our st and dt yields from the wrong tag combinations ( incorrect combinations that , by chance , lie within the @xmath109 signal region ) , we use the tag invariant mass sidebands . \\n we define the signal region as @xmath110 mev @xmath111 mev , and the sideband regions as @xmath112 mev @xmath113 mev or @xmath114 mev @xmath115 mev , where @xmath116 is the difference between the tag mass and the nominal mass . \\n we fit the st @xmath109 distributions to the sum of double - gaussian signal function plus second - degree chebyshev polynomial background function to get the tag mass sideband scaling factor . \\n the invariant mass distributions of tag candidates for each tag mode are shown in fig . \\n [ fig : dm ] and the st yield and @xmath109 sideband scaling factor are summarized in table  [ table : data - single ] . \\n we find @xmath117 summed over the three tag modes . \\n .[table : data - single ] summary of single - tag ( st ) yields , where @xmath118 is the yield in the st mass signal region , @xmath119 is the yield in the sideband region , @xmath120 is the sideband scaling factor , and @xmath68 is the scaled sideband - subtracted yield . [ cols=\"<,>,>,>,>\",options=\"header \" , ]     we considered six semileptonic decays , @xmath121 @xmath122 , @xmath123 , @xmath124 , @xmath125 , @xmath126 , and @xmath127 , as the major sources of background in the @xmath128 signal region . \\n the second dominates the nonpeaking background , and the fourth ( with @xmath129 ) dominates the peaking background . \\n uncertainty in the signal yield due to nonpeaking background ( @xmath130 ) is assessed by varying the semileptonic decay branching fractions by the precision with which they are known  @xcite . \\n imperfect knowledge of @xmath131 gives rise to a systematic uncertainty in our estimate of the amount of peaking background in the signal region , which has an effect on our branching fraction measurement of @xmath132 . \\n we study differences in efficiency , data vs mc events , due to the extra energy requirement , extra track veto , and @xmath133 requirement , by using samples from data and mc events , in which _ both _ the @xmath134 and @xmath2 satisfy our tag requirements , i.e. , `` double - tag \\'\\' events . \\n we then apply each of the above - mentioned requirements and compare loss in efficiency of data vs mc events . in this way \\n we obtain a correction of @xmath135 for the extra energy requirement and systematic uncertainties on each of the three requirements of @xmath136 ( all equal , by chance ) . \\n the non-@xmath69 background in the signal @xmath69 candidate sample is negligible ( @xmath137 ) due to the low probability ( @xmath138 per track ) that hadrons ( @xmath139 or @xmath140 ) are misidentified as @xmath69  @xcite . \\n uncertainty in these backgrounds produces a @xmath141 uncertainty in the measurement of @xmath142 . \\n the secondary @xmath69 backgrounds from charge symmetric processes , such as @xmath143 dalitz decay ( @xmath144 ) and @xmath145 conversion ( @xmath146 ) , are assessed by measuring the wrong - sign signal electron in events with @xmath147 . the uncertainty in the measurement from this source \\n is estimated to be @xmath148 . \\n other possible sources of systematic uncertainty include @xmath68 ( @xmath137 ) , tag bias ( @xmath149 ) , tracking efficiency ( @xmath148 ) , @xmath59 identification efficiency ( @xmath150 ) , and fsr ( @xmath150 ) . combining all contributions in quadrature , \\n the total systematic uncertainty in the branching fraction measurement is estimated to be @xmath151 . \\n in summary , using the sample of @xmath152 tagged @xmath28 decays with the cleo - c detector we obtain the absolute branching fraction of the leptonic decay @xmath153 through @xmath154 @xmath155 where the first uncertainty is statistical and the second is systematic . \\n this result supersedes our previous measurement  @xcite of the same branching fraction , which used a subsample of data used in this work . \\n the decay constant @xmath33 can be computed using eq . \\n ( [ eq : f ] ) with known values  @xcite @xmath156 gev@xmath157 , @xmath158 mev , @xmath159 mev , and @xmath160 s. we assume @xmath161 and use the value @xmath162 given in ref . \\n we obtain @xmath163    combining with our other determination  @xcite of @xmath164 mev with @xmath43 and @xmath0 ( @xmath165 ) decays , we obtain @xmath166 this result is derived from absolute branching fractions only and is the most precise determination of the @xmath91 leptonic decay constant to date .    our combined result is larger than the recent lqcd calculation @xmath167 mev  @xcite by @xmath168 standard deviations . \\n the difference between data and lqcd for @xmath33 could be due to physics beyond the sm  @xcite , unlikely statistical fluctuations in the experimental measurements or the lqcd calculation , or systematic uncertainties that are not understood in the lqcd calculation or the experimental measurements .    combining with our other determination  @xcite of @xmath169 , via @xmath44 \\n , we obtain @xmath170 using this with our measurement  @xcite of @xmath171 , we obtain the branching fraction ratio @xmath172 this is consistent with @xmath173 , the value predicted by the sm with lepton universality , as given in eq . \\n ( [ eq : f ] ) with known masses  @xcite . \\n we gratefully acknowledge the effort of the cesr staff in providing us with excellent luminosity and running conditions . \\n d.  cronin - hennessy and a.  ryd thank the a.p .  sloan foundation . \\n this work was supported by the national science foundation , the u.s . \\n department of energy , the natural sciences and engineering research council of canada , and the u.k . \\n science and technology facilities council .        c.  amsler \\n _ et al . _ \\n ( particle data group ) , phys . \\n b * 667 * , 1 ( 2008 ) . \\n k.  ikado _ et al . _ \\n ( belle collaboration ) , phys . \\n lett .   * 97 * , 251802 ( 2006 ) . \\n b.  aubert _ et al . \\n _ ( babar collaboration ) , phys .  rev . \\n d * 77 * , 011107 ( 2008 ) . \\n a.  g.  akeroyd and c.  h.  chen , phys . \\n d * 75 * , 075004 ( 2007 ) ; a.  g.  akeroyd , prog . \\n phys .   * 111 * , 295 ( 2004 ) . \\n j.  l.  hewett , arxiv : hep - ph/9505246 . \\n w.  s.  hou , phys . \\n d * 48 * , 2342 ( 1993 ) . \\n e.  follana , c.  t.  h.  davies , g.  p.  lepage , and j.  shigemitsu ( hpqcd collaboration ) , phys . \\n lett .   * \\n 100 * , 062002 ( 2008 ) . \\n b.  i.  eisenstein _ et al . \\n _ ( cleo collaboration ) , phys .  rev . \\n d * 78 * , 052003 ( 2008 ) . \\n b.  a.  dobrescu and a.  s.  kronfeld , phys . \\n * 100 * , 241802 ( 2008 ) . \\n d.  cronin - hennessy _ et al . \\n _ ( cleo collaboration ) , arxiv:0801.3418 . \\n m.  artuso _ et al . _ \\n ( cleo collaboration ) , phys . \\n lett .   * 99 * , 071802 ( 2007 ) . \\n k.  m.  ecklund _ et al . _ \\n ( cleo collaboration ) , phys .  rev . \\n lett .   * 100 * , 161801 ( 2008 ) . \\n j.  p.  alexander _ et al . \\n _ ( cleo collaboration ) , phys .  rev . \\n d * 79 * , 052001 ( 2009 ) . \\n y.  kubota _ et al . \\n _ ( cleo collaboration ) , nucl . \\n instrum . \\n a * 320 * , 66 ( 1992 ) . \\n d.  peterson _ \\n et al . _ , \\n instrum . \\n methods phys . \\n , sec .  a * 478 * , 142 ( 2002 ) . m.  artuso _ et al . _ , \\n nucl .  instrum . \\n methods phys . \\n a * 502 * , 91 ( 2003 ) . \\n s.  dobbs _ et al . \\n _ ( cleo collaboration ) , phys .  rev . \\n d * 76 * , 112001 ( 2007 ) . \\n j.  p.  alexander _ et al . \\n _ ( cleo collaboration ) , phys .  rev . \\n lett .   * 100 * , 161804 ( 2008 ) . \\n e.  barberio and z.  was , comput . \\n . commun . * 79 * , 291 ( 1994 ) .', 'abstract': 'we have studied the leptonic decay @xmath0 , via the decay channel @xmath1 , using a sample of tagged @xmath2 decays collected near the @xmath3 peak production energy in @xmath4 collisions with the cleo - c detector . \\n we obtain @xmath5 and determine the decay constant @xmath6  mev , where the first uncertainties are statistical and the second are systematic .'}\n"
          ]
        }
      ]
    },
    {
      "cell_type": "code",
      "source": [
        "from datasets import load_metric\n",
        "\n",
        "metric = load_metric(\"rouge\")\n",
        "\n",
        "\n",
        "batch_count = 0\n",
        "batches = []\n",
        "lex_rank_summarizer = LexRankSummarizer()\n",
        "print(small_eval_dataset[0])\n",
        "index = 0\n",
        "\n",
        "text_data = [] #articles\n",
        "summaries = []\n",
        "abstracts = []\n",
        "length_article = []\n",
        "length_summary = []\n",
        "length_abstract = []\n",
        "rouge_scores = []\n",
        "data = []\n",
        "for sample in tqdm(small_eval_dataset):\n",
        "    index+=1\n",
        "    # remove newline characters from each sample as we need to use exclusively as seperators\n",
        "    print(\"abstract\")\n",
        "    abstract = sample['abstract']\n",
        "    print(abstract)\n",
        "    abstracts.append(abstract)\n",
        "    length_abstract.append(get_num_words(abstract))\n",
        "\n",
        "    sample = sample['article'].replace('\\n', '')\n",
        "    parser = PlaintextParser.from_string(sample, Tokenizer(\"english\"))\n",
        "    lexrank_summary = lex_rank_summarizer(parser.document,sentences_count=5)\n",
        "\n",
        "    text_data.append(sample)\n",
        "    length_article.append(get_num_words(sample))\n",
        "    print(\"Lex Rank Summary\")\n",
        "    summary = \"\"\n",
        "    for sentence in lexrank_summary:\n",
        "      print(sentence)\n",
        "      summary += str(sentence)\n",
        "    summaries.append(summary)\n",
        "    length_summary.append(get_num_words(summary))\n",
        "    data.append([summary, sample, abstract, get_num_words(summary), get_num_words(sample), get_num_words(abstract)])\n",
        "\n",
        "baseline_rouge = metric.compute(predictions=summaries, references=abstracts)\n",
        "\n",
        "output = pd.DataFrame(data, columns = ['Summary', 'Article', 'Abstract', 'Summary Length', 'Article Length', 'Abstract Length'])\n",
        "#output2 = pd.DataFrame({'Summary': summaries, 'Article': text_data, 'Abstract': abstracts, 'Summary Length': length_summary, 'Article Length': length_article,'Abstract Length': length_abstract})\n",
        "\n",
        "print(\"HELLO\")\n",
        "output['Summary'][0]\n",
        "output['Abstract'][0]\n",
        "output"
      ],
      "metadata": {
        "colab": {
          "base_uri": "https://localhost:8080/",
          "height": 1000,
          "referenced_widgets": [
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            "a79ae9cfdaac44eab85465ef73202a75",
            "303800c44d1b469b8d6f2ac2d204afbe",
            "f5f72686bf07483e95b31e67990d1211",
            "2b66a6fc905a4a39b0bc47442649fd04",
            "f2a4ae74e4534657bb9dbcbdfa5462cc",
            "00b8e47facf14035885005abc851b342",
            "1ff18f48212b4e8ba47c446f8681a5f7",
            "065bfa38caf6480cb70a3237cef743b6"
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        },
        "id": "s84LeX9TVJqR",
        "outputId": "a84980fe-a98d-47be-fbf2-704bdd14fa05"
      },
      "execution_count": null,
      "outputs": [
        {
          "metadata": {
            "tags": null
          },
          "name": "stdout",
          "output_type": "stream",
          "text": [
            "{'article': \"with the discovery of fe  k@xmath0  emission at 6.4  kev  and spectral hardening at 2030  kev  in the x - ray spectra of seyfert  1 galaxies ( pounds et al . \\n 1990 ) , it was a center figure in probing the physics around black holes.ascas observation about the mcg-6 - 30 - 15 s board and skewed profile reveal two important physical mechanisms - the gravitational and the doppler effect.there are also other sources which show board and skewed profile.various explanation and observation about the fe  k@xmath0have been presented ( see fabian 2000,reynolds & nowak 2003 for details.)another intriguing thing is that , the sources always show a x - ray continuum with power - law distribution , till now , there is no convincing explanation about the production of the x - ray continuum .    from both the observational and theoretical side , \\n the iron line is expected to be the reflection from the accretion disk .a lot of computational method to compute the iron line profile from the vicinity of black hole has been invited(fanton 1997,bromley 1994,labor 1991),among which the most renowned is the ray - tracing method due to it s efficiency in computing.the differences in the line profiles from source to source have possibly implied variation in the geometry , the view angle , the structure of the bh - accretion disk system.with xmm s high s / n data , it greatly facilitate the astronomical community to study the iron k@xmath0 in agn . in order to model the fe  k@xmath0many detailed calculations about the accretion disk \\n must be performed.many author have make computation considering the geometry , such as flat , concave , conical , thick.(hartnoll 2002),merloni founded that the inner boundary condition of accretion flows have a significant effect on the profile . \\n the ionization state and fe abundance in the accretion disk also have been studied by ballantyne 1999,fabian 2002.nayakshins two - layer model in the surface of accretion disk also seems plausible.recent mhd studies have proposed that there may be exist spiral velocities in accretion disk which will brought quasi - humps in the profiles . \\n however , for simplicity , the disk emissivity is usually assumed to have a power - law profile @xmath1(where @xmath2 is the distance from the center in units of schwarzshild radii),and the index of such power - law is generally assumed to be given by the accretion disc emissitvity index in a standard geometrically thin and optically think disk(shakura sunyaev 1973).the fact that both wilms et al.2001 and miller et al.2002 require a larger value of @xmath0 to fit the line profile has prompted speculation that , in the inner disc disc region , additional energy dissipation must be taking place.the long mcg-6 - 30 - 15 s observation with xmm - newton reported by fabian et al.2002 show that , the strong , skewed iron line is clearly detected and is well characterized by a steep emissity profile within 6gm / c@xmath3 and a flatter profile beyond . \\n in contrast to explain the steep profile in the non - zero torque theory , which needs a comprehensive study of the mhd in accretion disk.we just make the simplest computation to deduced the flux striking the surface of the disk in the gr scheme , hence see the effects on line profiles , and the result is very useful in accounting for the steep emissivity in the inner part of the disk . \\n numerical models of reflection spectra from accretion discs began with the simplest case : assuming a static , neutral and constant density slab of material irradiated by a power - law continuum of x - rays . \\n george & fabian ( 1991 ) and matt , perola & piro ( 1991 ) performed monte - carlo calculations of the reflection spectra in such circumstances , and provided predictions on the equivalent width ( ew ) of fe  k@xmath0  for different reflection geometries.in this paper , we also assume the source is centredly located , static with a power law flux @xmath4,and this assumption is very close to the observation about the x - ray continuum . \\n the gravitational field of a rotating black hole is described by the kerr metric(we use units c = g=1 ) @xmath5 where @xmath6 @xmath7 @xmath8    we can see that the metric depends only on two parameters , the mass @xmath9 of the black hole and the specific angular momentum @xmath10 . and it is straight forward to formulate that the photo in kerr metric should has the relation in different place.we assume the photo propagate from place@xmath11to place@xmath12 then we can get @xmath13 and due to the invariance in general relativity @xmath14 so we can deduce that @xmath15 notice here , in the photons prorating in the kerr metric , the a is changing , due to the frequency changing.so we can get @xmath16 as we know , in the newtonian space - time the intensity of the flux should not be changed , how ever , eq .  [ intense ] show that the intensity changed due to a factor.the same , we can get @xmath17 where @xmath18is the flux striking the disc in kerr metric , while@xmath19is the fomat in newtonian space - time . in the newtonian space-time.in the model of point like , static source up the black hole \\n , the flux striking the disk should be @xmath20 in kerr black hole , we know that @xmath21 we set r , a , in unit of m , then@xmath19can have the detailed formula @xmath22 for a non - rotating black hole , we can get @xmath23 when we set r , h in unit of schwichild radii @xmath24,the formula change to @xmath25 from eq . \\n [ qin ] we can see that the flux striking the accretion disc has a close relation with both the photo index @xmath0 , the accretion rate @xmath26,and the sources location.observations shows that the source x - ray continuum always have a photo index @xmath27 . \\n when we compute the @xmath18 in this model , we find that in a extremely rotating kerr metric the flux concentrated on only a very small region near the center , while other place left nearly no illumination at all.it is apparently a gr effect.when it comes to the schwchild metric , the power law approximation is also not good to describe the emissivity , but it is rather flatter to the case in kerr metric.we can conclude that the need of steep power law model may due to a rapidly rotating black hole . \\n our work is invoked by recent report of steep emissity in inner part of accretion disk(fabian 2002).in the observation of mcg-6 - 30 - 15,fabian use a broken emissivity law to model the data , and with good result.however,they assume that the steep emissivity is a result from two reflector in the disk . in our work \\n we can see that , the steep emissivity may come from the effect of light bending near the center black hole.and the concentrating of flux , will give inner side a rather high ionization parameter,@xmath28 , which may result a line component at @xmath29kev.there are also other sources , such as iras 13224 - 3809(boller 2003),which should induce a steeper emissivity law.the steep emissivity law may be a evidence of a centering rapidly rotating black hole .    in present x - ray study , \\n there are lots of uncertainty in modelling the iron lines in agn , the s / n is a big problem to determine the real shape of the line.former observation confirms that there exist many agn which contain board and skew iron line , indicating that the line is produced very near the black hole.however,recent xmm observation show that there does not ubiquitous exist board iron line , instead , a narrow cole at 6.4 kev is present.this has not been included in this paper .    our work show that in the gr effect , the emissity can not be simply regarded as a power law as a function of r , instead , it should be described by various factors such as a , the source s position the photo index.when computed in the gr we find in the kerr metric the large concentration of the flux in the accretion disc , rather left other part of the disk `` empty'',also , the large concentration in flux will undoubtedly invoke the model of ionized disk describe by ross 1999.and our work is only a simplified model to test the gr effects , further work such as the disk motion and density under high illumination which may affect the emissity should be invoked . \\n ballantyne d.r . \\n , fabian a.c . , 2001 , mnras , 328 , l11 ballantyne d.r . , \\n ross r.r , 2002 , mnras , in press ( astro - ph/0201420 ) ballantyne d.r . \\n , fabian a.c . , ross r.r . , 2002 , mnras , 329 , l67 ballantyne d.r . , iwasawa k. , fabian a.c . , 2001 , mnras , 323 , 506 ballantyne d.r . , ross r.r . \\n , fabian a.c . , 2001 , \\n mnras , 327 , 10 boller th . \\n , brandt w.n . , fink h.h . , 1996 , a&a , 305 , 53 branduardi - raymont g. , sako m. , kahn s.m . \\n , brinkman a.c . , \\n kaastra j.s . \\n , page m.j . , 2001 , a&a , 365 , l140 \\n george i.m . \\n , fabian a.c . , 1991 , mnras , 249 , 352 ( fabian)fabian a.c , vaughan.s , nandra k , iwasawa k , ballantyne d.r , lee j.c , a de rosa , turner , & yound a.j,2002 mnras matt g. , perola g.c . , piro l. , 1991 , a&a , 247 , 27 matt g. , fabian a.c . , \\n ross r.r . , 1993 , mnras , 262 , 179 matt g. , fabian a.c . , ross r.r . , 1996 , mnras , 278 , 1111 matt g. , fabian a.c . , reynolds c.s . , 1997 , mnras , 289 , 175 nayakshin s. , kallman t.r . , 2001 , apj , 546 , 406 nayakshin s. , kazanas d. , 2002 , apj , 567 , 85 nayakshin s. , kazanas d. , kallman t. , 2000 , apj , 537 , 833    ross r.r . , fabian a.c \\n , 1993 , mnras , 261 , 74 ross r.r . , fabian a.c . , young a.j \\n . , 1999 , mnras , 306 , 461 raska a. , 1999 , mnras , 308 , 751 raska a. , czerny b. , 1996 , acta astronomica , 46 , 233 shakura n.i . , sunyaev r.a . , 1973 , \\n a&a , 24 , 337 tanaka y. , et al . , 1995 , nature , 344 , 747 vaughan s. , pounds k.a . , reeves j. , warwick r. , edelson r. , 1999 , mnras , 308 , l34\", 'abstract': 'in this paper , we present a simple relativistic approach to analyze the flux striking the disk which is possibly from a source up the black hole.the x - ray source is locate above an accretion disc orbiting around the black hole , this assumption is invoked by recent studies about iron k@xmath0 . we compute and arguing that due to the light bending effect near black hole , the flux striking the disk surface may be very concentrated , which will undoubtable change the disk s ionization state hence change the iron line s ionization state and emissivity.also,our model may explain the steep power law when modelling the lines .'}\n"
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            "abstract\n",
            "in this paper , we present a simple relativistic approach to analyze the flux striking the disk which is possibly from a source up the black hole.the x - ray source is locate above an accretion disc orbiting around the black hole , this assumption is invoked by recent studies about iron k@xmath0 . we compute and arguing that due to the light bending effect near black hole , the flux striking the disk surface may be very concentrated , which will undoubtable change the disk s ionization state hence change the iron line s ionization state and emissivity.also,our model may explain the steep power law when modelling the lines .\n",
            "111\n",
            "1865\n",
            "Lex Rank Summary\n",
            "however , for simplicity , the disk emissivity is usually assumed to have a power - law profile @xmath1(where @xmath2 is the distance from the center in units of schwarzshild radii),and the index of such power - law is generally assumed to be given by the accretion disc emissitvity index in a standard geometrically thin and optically think disk(shakura sunyaev 1973).the fact that both wilms et al.2001 and miller et al.2002 require a larger value of @xmath0 to fit the line profile has prompted speculation that , in the inner disc disc region , additional energy dissipation must be taking place.the long mcg-6 - 30 - 15 s observation with xmm - newton reported by fabian et al.2002 show that , the strong , skewed iron line is clearly detected and is well characterized by a steep emissity profile within 6gm / c@xmath3 and a flatter profile beyond .\n",
            "george & fabian ( 1991 ) and matt , perola & piro ( 1991 ) performed monte - carlo calculations of the reflection spectra in such circumstances , and provided predictions on the equivalent width ( ew ) of fe  k@xmath0  for different reflection geometries.in this paper , we also assume the source is centredly located , static with a power law flux @xmath4,and this assumption is very close to the observation about the x - ray continuum .\n",
            ", fabian a.c . , 2001 , mnras , 328 , l11 ballantyne d.r .\n",
            ", 1993 , mnras , 262 , 179 matt g. , fabian a.c . , ross r.r .\n",
            ", fabian a.c  , 1993 , mnras , 261 , 74 ross r.r .\n",
            "271\n",
            "271\n",
            "1865\n",
            "111\n",
            "abstract\n",
            "the first well - localized short - duration gamma ray bursts ( grbs ) , grb 050509b , grb 050709 and grb 050724 , could have been the narrowly beamed initial spike of a burst / hyper flare of soft gamma ray repeaters ( sgrs ) in host galaxies at cosmological distances . \n",
            " such bursts are expected if sgrs are young hyperstars , i.e. neutron stars where a considerable fraction of their neutrons have converted to hyperons and/or strange quark matter .    -1 cm\n",
            "84\n",
            "4966\n",
            "Lex Rank Summary\n",
            "the leading scenarios for the origin of short grbs , include , ( a ) merger of neutron - star ( ns ) or black hole ( bh ) binaries ( goodman et al .  1987 ; eichler et al .  1989 ; mochkovitch et al .  1993 ) , ( b ) gravitational collapse of accreting white dwarf ( dar & de rjula  2003;2004 ) , ( c ) gravitational collapse of neutron stars to strange - quark stars ( dar  1999 ) or hyperstars ( dar & de rjula  2000 ) and ( d ) giant flares from soft gamma ray repeaters ( sgrs ) in external galaxies ( dado et al .  2005 ; hurley et al .  2005 ) .\n",
            "rather than adopting a specific model  , we will assume that sgrs are hyperstars with a gravitational mass similar to that of canonical ns s , @xmath57 and with a radius significantly smaller than that of ns s , and that their energy source is gravitational contraction induced by the transition from neutron matter to hyper matter .\n",
            "the best supportive evidence that the slowly rotating sgrs and axps are hyperstars with a radius significantly smaller than that of ordinary radio pulsars , may come from the black body component of their persistent emission ( dar and de rjula  2000 ) and/or from the redshift of @xmath58 annihilation line if emitted near their surface .\n",
            "* grbs from the birth of sgrs / hyperstars : * the total energy release in the transition of an ns to a hyper star is @xmath67 of the gravitational energy release , because @xmath18 half of the gravitational energy release is used to increase the pressure and energy of the fermi gas .\n",
            "( [ eiso],[dop ] ) yield @xmath102 thus , if the initial short spike of sgr 1806 - 20 on december 27 , 2004 with @xmath103 was produced by a relativistic jet , which was viewed from an angle @xmath104 , it could have been seen at a redshift @xmath105 as a short grb with an isotropic energy @xmath106 similar to that of the short grbs 050509b , 050709 and 050724 , if its viewing angle was smaller by a factor @xmath18 3 .  note that this is independent of the value of @xmath3 provided that @xmath107  long duration grbs seem to be produced by highly relativistic jets ejected from mass accretion on a proto - neutron star or a black hole in core collapse sn explosions ( see , e.g. dar and de rjula  2004 ) .\n",
            "427\n",
            "427\n",
            "4966\n",
            "84\n",
            "abstract\n",
            "we estimate the critical magnetic field strength at which the lowest or second landau levels play an important role in the quark phase inside the hybrid stars , and show that the magnetic field should be in the order of @xmath0 gauss at the nuclear density @xmath1 @xmath2 . \n",
            " we also find that the pressure of quark matter settling only in the lowest landau level can be expressed as a function of the energy density independently of the magnetic field strength , which corresponds to the causality limit of a stiff equation of state . \n",
            " adiabatic index of quark matter well exceeds 4/3 in the core , and we find a possibility to construct massive hybrid star models occupied in large part by quark matter , whose maximum mass becomes larger than two solar mass . \n",
            " [ firstpage ]    relativity  stars : neutron\n",
            "143\n",
            "2861\n",
            "Lex Rank Summary\n",
            "inside the hybrid star  , one has only to consider three flavor quark matter composed of @xmath15 , @xmath16 , and @xmath17 quarks , because the more massive quarks can not be produced under the typical energy density of neutron stars .\n",
            "we derive a critical magnetic field @xmath22 for given density , above which only the lowest landau level is occupied , and find the eos becomes stiffest as a causality limit for @xmath23 , independent of the magnetic field .\n",
            "thus , the condition for all quarks only occupy lll is given by that the magnetic field should be stronger than the critical strength for @xmath16 and @xmath17 quarks , i.e. , one can show that the magnetic field strength should be larger than the critical strength @xmath22 given by @xmath67{6\\pi^4}\\hbar c}{e}n_{\\rm b}^{2/3 } \\nonumber \\\\             & = & 1.62\\times 10^{19 } \\times\\left(\\frac{n_{\\rm b}}{n_0}\\right)^{2/3 } \\  \\rm{gauss}.\n",
            "as a result , we find that the stellar model constructed with eos connected to the hadronic matter at the lower energy density can realize more massive stellar model with smaller central energy density .\n",
            "that is , the central strength of magnetic field can not reach to the critical magnetic field strength to realize the landau effects in quark matter phase even for magnetar with @xmath104 gauss , if the magnetic field configuration inside the star would be simply dipole .\n",
            "227\n",
            "227\n",
            "2861\n",
            "143\n",
            "abstract\n",
            "the reuven ramaty high energy solar spectroscopic imager ( rhessi ) has been observing gamma - ray lines from the sun and the galaxy since its launch in february 2002 . here \n",
            " i summarize the status of rhessi observations of solar lines ( nuclear de - excitation , neutron capture , and positron annihilation ) , the lines of @xmath0al and @xmath1fe from the inner galaxy , and the search for positron annihilation in novae . \n",
            " [ 2001/04/25 1.1 ( pwd ) ]\n",
            "83\n",
            "3190\n",
            "Lex Rank Summary\n",
            "imaging is therefore limited to 35  at the 2.223  mev line from neutron capture in solar flares , and to 3 for the 4 and 6 mev lines from carbon and oxygen de - excitation .\n",
            "for photons on the order of 1  mev or higher , in fact  , the instrument s effective area ( about 29 @xmath3 at 1809 kev ) has little dependence on the direction of incidence , with the exception of a @xmath430% depression at near - solar angles due to the effects of the grids , absorption in the front segments , and opacity of parts of the spacecraft bus .\n",
            "the results reported in that volume are summarized in @xcite , and include :    * the discovery @xcite that the 2.223  mev neutron - capture line in this flare , a good tracer of the interactions of accelerated ions , was centered at a position significantly offset from the distribution of hard x - rays from electron bremsstrahlung .\n",
            "i reported the @xmath0al flux for the first nine months of the _ rhessi _ mission to be @xmath11 ph  @xmath12  s@xmath13 @xcite , comparable to the value found by the gris balloon @xcite but significantly higher than the sum of the comptel map in this range of galactic longitude @xcite .\n",
            "by studying these lines , particularly the line of @xmath17k ( which will have a constant flux throughout the mission since it is a natural radioactivity )  , we can determine the effect that radiation damage has on the measured flux for a gaussian fit .\n",
            "260\n",
            "260\n",
            "3190\n",
            "83\n",
            "abstract\n",
            "symbiotic stars are long - period interacting binary systems in which an evolved red giant star transfers material to its much hotter compact companion \n",
            " . such a composition places them among the most variable stars . \n",
            " in addition to periodic variations due to the binary motion they often show irregular changes due to nova - like eruptions of the hot component . in some systems the cool giant is a pulsating mira - type star usually surrounded by a variable dust shell . \n",
            " here , i present results of optical and ir monitoring of symbiotic systems as well as future prospects for such studies .\n",
            "105\n",
            "2952\n",
            "Lex Rank Summary\n",
            "the cool giant can also show intrinsic variability , in particular , radial pulsations ( all d - type and some s - type systems ) and semi - regular variations ( s - type ) with timescales of order of months and years as well as long - term light variations due to variable obscuration by circumstellar dust ( most d - type systems ) , solar - type cycles , spots , etc .\n",
            "in addition , the hot components in many systems show activity with timescales of a few years which can not be simply accounted for by the thermonuclear models .\n",
            "both the light curves and the radial velocity curves show multiple periodicities : a @xmath24 photometric period , best visible in the @xmath19 light curves , has been attributed to radial pulsation of the giant ( mikoajewski , mikoajewska , & khudyakova 1992 ) , while the nature of the secondary period of @xmath25 also present in the radial velocity curve is not clear ( hinkle et al .  1993 ; munari et al .  there is a controversy about whether the system is triple or binary , and whether the symbiotic pair is the inner binary or the white dwarf is on the longer orbit .\n",
            "the near - ir light curves also show long - term variations similar to the dust obscuration phenomena found in symbiotic miras ( cf .\n",
            "it is possible that the main difference between ci cyg , z and , ax per , and other related symbiotic systems with multiple eruption activity and the activity of accretion - powered systems ( symbiotic recurrent novae and ch cyg ) is that the hot component in the former burns more or less stably the accreted hydrogen whereas not in the latter .\n",
            "297\n",
            "297\n",
            "2952\n",
            "105\n",
            "abstract\n",
            "quasiparticle states around a single vortex in a @xmath0-wave superconductor are studied on the basis of the bogoliubov - de gennes ( bdg ) theory , where both charge and current screenings are taken into account . due to the violation of time reversal symmetry , \n",
            " there are two types of vortices which are distinguished by their winding orientations relative to the angular momentum of the chiral cooper pair . \n",
            " the bdg solution shows that the charges of the two types of vortices are quite different , reflecting the rotating cooper pair of the @xmath0-wave paring state .\n",
            "98\n",
            "4130\n",
            "Lex Rank Summary\n",
            "[ fig:1](a ) .\n",
            "contrary to the c - vortex , the electron density is almost uniform at all temperatures for the u - vortex , so that the vortex charge is very small in this case .\n",
            "[ fig:3](a ) ] .\n",
            "we note that the electron density for the u - vortex is very similar to that for the c - vortex at @xmath85 , where the @xmath77 state is occupied .\n",
            "for the c - vortex  the bound state energy is positive for @xmath75 , while it is negative or zero for the u - vortex .\n",
            "96\n",
            "96\n",
            "4130\n",
            "98\n",
            "abstract\n",
            "we present a study on the charge current quasi elastic scattering of @xmath0 from nucleon and nuclei which gives a charged muon in the final state . to describe nuclei , \n",
            " the fermi gas model has been employed with pauli suppression factor . \n",
            " the diffuseness parameter of the fermi distribution and binding energy of nucleons inside the nuclei have been used as parameters . \n",
            " we also investigate different parametrizations for electric and magnetic sach s form factors of nucleons . \n",
            " calculations have been made for ccqes total and differential cross sections for the case of @xmath1 , @xmath2 and @xmath3 scattering and are compared with the data for different values of the axial mass . \n",
            " the present model gives excellent description of measured differential cross section . \n",
            " the nuclear effects reduce the cross section by 10 % even at higher neutrino energy above 1 gev .    _ quasi elastic scattering , neutrino - nucleus interaction , fermi model _\n",
            "159\n",
            "3434\n",
            "Lex Rank Summary\n",
            "the sach s form factor given by alberico et al.@xcite are @xmath53 we study the effect of galster and alberico parametrizations of electromagnetic form factors on ccqes cross section of neutrino nucleon scattering .\n",
            "* the fermi gas model *    the cross section for the neutrino scattering with a nucleon in a nucleus is smaller than that in case of a free nucleon scattering .\n",
            "for @xmath1 , @xmath2 and @xmath3 ccqes as a function of @xmath91 at neutrino energy @xmath26 = 2 for axial mass @xmath37 = 1.05 gev.,scaledwidth=100.0% ]     for @xmath1 , @xmath2 and @xmath3 ccqes as a function of @xmath91 at neutrino  energy @xmath26 = 2 for axial mass @xmath37 = 1.05 gev.,scaledwidth=100.0% ]    figure [ figure7_neutrino_carbon_differential_xsection_neutrino_788_mev ] shows the differential cross section @xmath90 per neutron for the neutrino - carbon ccqes qes as a function of @xmath91 at different values of axial mass @xmath37= 0.979 , 1.05 , 1.12 and 1.23 gev using galster parametrizations for sach s form factors .\n",
            "figure [ figure14_neutrino_iron_total_cross_section ] shows the total cross section @xmath95 per neutron for the neutrino - iron ccqes as a function of the @xmath26 obtained using galster parametrization with axial mass @xmath37= 0.979 , 1.05 , 1.12 and 1.23 gev .\n",
            "per neutron for the neutrino - iron charged current quasi elastic scattering as a function of neutrino energy @xmath26 for different values of the axial mass @xmath37 compared with the data @xcite.,scaledwidth=100.0% ]     per neutron for the neutrino - iron charged current quasi elastic scattering as a function of neutrino energy @xmath26 for different values of the axial mass @xmath37 compared with the data @xcite.,scaledwidth=100.0% ]  we presented a study on the charge current quasi elastic scattering of @xmath0 from nucleon and nuclei .\n",
            "286\n",
            "286\n",
            "3434\n",
            "159\n",
            "abstract\n",
            "we consider the `` two flavour '' nambu  jona - lasinio model in the presence of a vector and an axial external chemical potentials and study the phase structure of the model at zero temperature . \n",
            " the nambu  jona - lasinio model is often used as a toy replica of qcd and it is therefore interesting to explore the consequences of adding external vector and axial chemical potentials in this model , mostly motivated by claims that such external drivers could trigger a phase where parity could be broken in qcd . \n",
            " we are also motivated by some lattice analysis that attempt to understand the nature of the so - called aoki phase using this simplified model . \n",
            " analogies and differences with the expected behaviour in qcd are discussed and the limitations of the model are pointed out . \n",
            " iccub-13 - 229\n",
            "142\n",
            "7175\n",
            "Lex Rank Summary\n",
            "it turns out that the conditions for this phase to be stable and exhibit chiral symmetry breaking too are such that one gets an inverted mass spectrum with @xmath2 and @xmath3 , which is quite different from qcd .\n",
            "this plot shows that the njl with external drivers has a rather complex phase diagram.,title=\"fig : \" ]   depending on @xmath1 for different values of the chemical potential @xmath0 setting @xmath81 mev , @xmath80 and @xmath78 .\n",
            "thus parity breaking in the njl model corresponds to a choice of parameters that makes this model quite different from qcd predictions @xcite .\n",
            "we have investigated all the properties of the transition from the parity - even to the parity - odd phase providing results on the evolution of both condensates , which exhibit finite jumps under certain conditions , and finally examining the phase transition line , where it was shown that for @xmath146 we have a 2nd order transition while for @xmath137 , it corresponds to a 1st order one .\n",
            "b 678 ( 2009 ) 416 .  a. a. andrianov , d. espriu , x. planells , eur .  . j c73 ( 2013 ) 2294    p. v. buividovich , m. n. chernodub , e. v. luschevskaya , m. i. polikarpov , phys .\n",
            "210\n",
            "210\n",
            "7175\n",
            "142\n",
            "abstract\n",
            "we present a monte carlo model for degradation of 1 - 10,000 ev electrons in an atmosphere of methane . the electron impact cross sections for ch@xmath0 are compiled and analytical representations of these cross sections are used as input to the model.``yield spectra '' , which provides information about the number of inelastic events that have taken place in each energy bin , is used to calculate the yield ( or population ) of various inelastic processes . \n",
            " the numerical yield spectra , obtained from the monte carlo simulations , is represented analytically , thus generating the analytical yield spectra ( ays ) . \n",
            " ays is employed to obtain the mean energy per ion pair and efficiencies of various inelastic processes . \n",
            " mean energy per ion pair for neutral ch@xmath0 is found to be 26 ( 27.8 ) ev at 10 ( 0.1 ) kev . \n",
            " efficiency calculation showed that ionization is the dominant process at energies @xmath150 ev , for which more than 50% of the incident electron energy is used . above 25 ev \n",
            " , dissociation has an efficiency of @xmath227% . \n",
            " below 10 ev , vibrational excitation dominates . \n",
            " contribution of emission is around 1.2% at 10 kev . \n",
            " efficiency of attachment process is @xmath20.1% at 8 ev and efficiency falls down to negligibly small values at energies greater than 15 ev . \n",
            " the efficiencies can be used to calculate volume production rate in planetary atmospheres by folding with electron production rate and integrating over energy . \n",
            " planetary atmospheres , molecular processes , monte carlo model , electron degradation , methane .\n",
            "266\n",
            "6594\n",
            "Lex Rank Summary\n",
            "the aim of this study is to present a monte carlo model which describes the degradation of electrons with energy in the range 1 ev to 10 kev in a ch@xmath3 atmosphere .\n",
            "measurements of @xcite are found to be lower than the values of @xcite by @xmath250% .\n",
            "it is calculated as @xmath68 where @xmath69 is the population of the @xmath70 process at the incident electron energy e@xmath29 .\n",
            "the efficiency , @xmath74 , of the @xmath70 process at the incident energy @xmath75 can be obtained as @xmath76 where @xmath77 is the threshold for the @xmath70 process .\n",
            "efficiencies are calculated using the ays as well as the nys , and are found to be in good agreement for energy @xmath110 ev .\n",
            "120\n",
            "120\n",
            "6594\n",
            "266\n",
            "abstract\n",
            "in smart grid , a home appliance can adjust its power consumption level according to the realtime power price obtained from communication channels . \n",
            " most studies on smart grid do not consider the cost of communications which can not be ignored in many situations . \n",
            " therefore , the total cost in smart grid should be jointly optimized with the communication cost . in this paper , \n",
            " a probabilistic mechanism of locational margin price ( lmp ) is applied and a model for the stochastic evolution of the underlying load which determines the power price is proposed . \n",
            " based on this framework of power price , the problem of determining when to inquire the power price is formulated as a markov decision process and the corresponding elements , namely the action space , system state and reward function , are defined . \n",
            " dynamic programming is then applied to obtain the optimal strategy . \n",
            " a simpler myopic approach is proposed by comparing the cost of communications and the penalty incurred by using the old value of power price . \n",
            " numerical results show the significant performance gain of the optimal strategy of price inquiry , as well as the near - optimality of the myopic approach .\n",
            "204\n",
            "3800\n",
            "Lex Rank Summary\n",
            "[ fig : model ] .\n",
            "we denote by @xmath0 the power price and @xmath1 the power consumption at the @xmath2-th time slot .\n",
            "therefore , the decision of power consumption is based on the power price of the previous price inquiry , i.e. @xmath1 is a function of @xmath10 .\n",
            "for time  slot @xmath2 , the system state is given by @xmath39 .\n",
            "if the action of the current time slot is 0 , i.e. no inquiry , the expected reward of the current time slot is given by ( recall that the power consumption level @xmath55 is a function of the assumed price ) @xmath56 otherwise , the reward is given by ( recalled that @xmath4 is the cost of communication ) @xmath57      once defining the elements of mdp , we can apply dynamic programming ( dp ) @xcite to obtain the optimal strategy .\n",
            "143\n",
            "143\n",
            "3800\n",
            "204\n",
            "abstract\n",
            "we compute the recoil polarization of the lambda - hyperon and the photon asymmetry for the quasifree photoproduction of kaons in a relativistic impulse - approximation approach . \n",
            " our motivation for studying polarization observables is threefold . \n",
            " first , polarization observables are more effective discriminators of subtle dynamics than the unpolarized cross section . \n",
            " second , earlier nonrelativistic calculations suggest an almost complete insensitivity of polarization observables to distortions effects . \n",
            " finally , this insensitivity entails an enormous simplification in the theoretical treatment . indeed , by introducing the notion of a `` bound - nucleon propagator '' we exploit feynman s trace techniques to develop closed - form , analytic expressions for all photoproduction observables . \n",
            " moreover , our results indicate that polarization observables are also insensitive to relativistic effects and to the nuclear target . \n",
            " yet , they are sensitive to the model parameters , making them ideal tools for the study of modifications to the elementary amplitude  such as in the production , propagation , and decay of nucleon resonances  in the nuclear medium .\n",
            "178\n",
            "4558\n",
            "Lex Rank Summary\n",
            "the differential cross section for the quasifree process is derived to be : @xmath15 where @xmath16 is the spin of the emitted @xmath2 , @xmath17 is the polarization of the incident photon , @xmath18 is the nucleon mass , and @xmath19 is the transition matrix element given by : @xmath20 here @xmath21 is the free dirac spinor for the emitted @xmath2-hyperon and @xmath22 is the fourier transform of the relativistic spinor for the bound nucleon ( @xmath23 denotes the collection of all quantum numbers necessary to specify the single - particle orbital ) .\n",
            "that is , @xmath25 yet , our prime interest in this work is the calculation of polarization observables : the recoil @xmath2-polarization ( @xmath26 ) and the photon asymmetry ( @xmath27 ) .\n",
            "[ fig2 ] we display the recoil polarization ( @xmath26 ) of the @xmath57hyperon and the photon asymmetry ( @xmath27 ) as a function of the kaon scattering angle for the knockout of a proton from the @xmath58 orbital in @xmath59c .\n",
            "having established the independence of polarization observables to the nuclear target and to relativistic effects  particularly for the case of the recoil polarization  we are now in a good position to discuss the sensitivity of these observables to the elementary amplitude ( note that the insensitivity of polarization observables to final - state interaction has been shown convincingly in ref .\n",
            "we have computed polarization observables  the recoil polarization of the @xmath2-hyperon and the photon asymmetry  for the quasifree @xmath54 photoproduction reaction from nuclei .\n",
            "250\n",
            "250\n",
            "4558\n",
            "178\n",
            "abstract\n",
            "we present a simple on - chip electronic thermometer with the potential to operate down to 1  mk . \n",
            " it is based on transport through a single normal - metal - superconductor tunnel junction with rapidly widening leads . \n",
            " the current through the junction is determined by the temperature of the normal electrode that is efficiently thermalized to the phonon bath , and it is virtually insensitive to the temperature of the superconductor , even when the latter is relatively far from equilibrium . \n",
            " we demonstrate here the operation of the device down to 7  mk and present a systematic thermal analysis .\n",
            "103\n",
            "5624\n",
            "Lex Rank Summary\n",
            "@xcite ) , where @xmath13 , and @xmath14 is the temperature of the superconductor .\n",
            "( [ eq.1 ] ) by @xmath25 where @xmath26 @xcite .\n",
            "we evaluate the influence of the @xmath11 parameter on the relative deviations of the present thermometer based on method @xmath32 numerically , as shown in fig .\n",
            "[ fig:1 ]  ( a ) and [ fig:5 ] ] .\n",
            "the heat released through @xmath134 = 2 bonding wires is @xmath135 , where its cross - sectional area is @xmath136 with a radius @xmath137 = 16 @xmath21 m .  the temperature obtained from both methods @xmath30 and @xmath32 is affected by less than 0.5 @xmath51 by self - heating of the normal metal down to a temperature of 1  mk .\n",
            "122\n",
            "122\n",
            "5624\n",
            "103\n",
            "abstract\n",
            "large - scale structure distorts the images of background galaxies , which allows one to measure directly the projected distribution of dark matter in the universe and determine its power spectrum . \n",
            " here we address the question of how to extract this information from the observations . \n",
            " we derive minimum variance estimators for projected density reconstruction and its power spectrum and apply them to simulated data sets , showing that they give a good agreement with the theoretical minimum variance expectations . \n",
            " the same estimator can also be applied to the cluster reconstruction , where it remains a useful reconstruction technique , although it is no longer optimal for every application . \n",
            " the method can be generalized to include nonlinear cluster reconstruction and photometric information on redshifts of background galaxies in the analysis . \n",
            " we also address the question of how to obtain directly the 3-d power spectrum from the weak lensing data . \n",
            " we derive a minimum variance quadratic estimator , which maximizes the likelihood function for the 3-d power spectrum and can be computed either from the measurements directly or from the 2-d power spectrum . \n",
            " the estimator correctly propagates the errors and provides a full correlation matrix of the estimates . \n",
            " it can be generalized to the case where redshift distribution depends on the galaxy photometric properties , which allows one to measure both the 3-d power spectrum and its time evolution . \n",
            " # 1\n",
            "238\n",
            "12154\n",
            "Lex Rank Summary\n",
            "the modes @xmath48 we wish to estimate are related to these through the relation @xmath113 and their covariance matrix is given by @xmath114 if we use these modes in the likelihood function ( equation [ lik ] ) and in the corresponding quadratic estimator ( equation [ wffll ] ) we reduce the matrix by a factor of two ( and the computational cost by a factor of eight ) , even if we use the same number of modes as the number of galaxies .\n",
            "wf estimator is give by equation ( [ wf ] ) with the variance of residuals @xmath126.\\ ] ] the bias and fisher matrix are given by latexmath:[\\ ] ]    the above expressions use all the distance information in an optimal way .\n",
            "if we reduce the size then the cluster becomes more important and the contribution from nongaussian modes to the power spectrum can dominate over the noise to smaller scales than in previous example , resulting in keeping more small scale modes in the reconstruction .\n",
            "it is possible to invert from the 2-d power spectrum or to compute directly from the data the 3-d power spectrum , which will also be unbiased and minimum variance .\n",
            "to apply wf one has to compute the power spectrum on the data first using the methods discussed above .\n",
            "221\n",
            "221\n",
            "12154\n",
            "238\n",
            "abstract\n",
            "in this talk we introduce our recent results of global 1d mhd simulations for the acceleration of solar and stellar winds . we impose transverse photospheric motions corresponding to the granulations , which generate outgoing alfvn waves . \n",
            " the waves effectively dissipate by 3-wave coupling and direct mode conversion to compressive waves in density - stratified atmosphere . \n",
            " we show that the coronal heating and the solar wind acceleration in the open magnetic field regions are natural consequence of the footpoint fluctuations of the magnetic fields at the surface ( photosphere ) . \n",
            " we also discuss winds from red giant stars driven by waves , focusing on different aspects from the solar wind . \n",
            " we show that red giants wind are highly structured with intermittent magnetized hot bubbles embedded in cool chromospheric material .\n",
            "134\n",
            "3027\n",
            "Lex Rank Summary\n",
            "because ( 1 ) the low - frequency wave is expected to have more power , and ( 2 ) the resonance frequency of  the proton is higher than those of heavier ions so that the energy of the ioncyclotron wave is in advance absorbed by heavy ions ( cranmer 2000 ) .\n",
            "although the energy flux , @xmath40erg @xmath41s@xmath11 , of the outgoing waves ( @xmath35 in the static region is equivalent with the energy flux ) which penetrates into the corona is only @xmath42% of the input value , it satisfies the requirement for the energy budget in the coronal holes ( withbroe & noyes 1977 ) .\n",
            "the properties of surface fluctuations ( e.g. amplitude and spectrum ) can be estimated from conditions of surface convection which depend on surface gravity and temperature ( e.g. renzini et al.1977 ; stein et al .  then , we carry out the simulations of the red giant winds in a similar manner to the solar wind simulations .\n",
            "we have shown that the dissipation of the low - frequency waves through the generation of the compressive waves ( decay instability ) and shocks ( nonlinear steepening ) is one of the solutions for the heating and acceleration of the plasma in the coronal holes .\n",
            ", 220 , 229 suzuki , t. k. , 2007 apj , 659 , 1592    suzuki , t. k. & inutsuka , s. , 2005 apj , 632 , l49 suzuki , t . k. & inutsuka , s. , 2006 j. geophys .\n",
            "255\n",
            "255\n",
            "3027\n",
            "134\n",
            "abstract\n",
            "in this paper we study the relation between the light - front ( infinite momentum ) and rest - frame descriptions of quarkonia . while the former is more convenient for high - energy production , the latter is usually used for the evaluation of charmonium properties . \n",
            " in particular , we discuss the dynamics of a relativistically moving system with nonrelativistic internal motion and give relations between rest frame and light - front potentials used for the description of quarkonium states . \n",
            " we consider two approximations , first the small coupling regime , and next the nonperturbative small binding energy approximation . in both cases we get consistent results \n",
            " . our results could be relevant for the description of final state interactions in a wide class of processes , including quarkonium production on nuclei and plasma . \n",
            " moreover , they can be extended to the description of final state interactions in the production of weakly bound systems , such as for example the deuteron .\n",
            "166\n",
            "4332\n",
            "Lex Rank Summary\n",
            "the dynamics of such systems is described in potential models , and the wave functions in different reference frames can be related to each other : it is well - known that in the light front quantization approach the wave function is invariant with respect to longitudinal boosts  @xcite , so a transformation of the rest frame wave function requires just to rewrite it in terms of light - front variables  @xcite .\n",
            "taking into account  that the projection of the vector @xmath26 on @xmath22 is @xmath27 ( this corresponds to a generalization of the rest frame instantaneous approximation @xmath28 ) , after some algebra ( see appendix  [ sec : bse_derivation ] ) we can obtain a schroedinger equation for the internal motion in the form @xmath29 where we defined a wave function @xmath30 as @xmath31 a potential @xmath32 is proportional to the trace of the gluon propagator , @xmath33 , where @xmath34 is the gluon propagator , and the derivatives are defined as @xmath35 here we introduced the shorthand notations @xmath36 , and @xmath37 for the mass of quarkonium .\n",
            "we would like to emphasize that in contrast to  @xcite the potential @xmath99 is local only in the coordinate space ; in a lf frame the interaction has a form of a convolution @xmath100 the green function of the internal motion in the infinite momentum frame satisfies an evolution equation @xmath101    finally , we would like to address how the light front and rest frame potentials are related to each other .\n",
            "also , we got that in the infinite momentum frame a potential is given by a convolution  ( [ eq : u_def],[eq : k_def ] ) in light - front variable @xmath83 , in contrast to what was found in  @xcite .\n",
            "if we denote @xmath126 and define small deviations as @xmath23 , we may expect that a deviation of quark momenta from @xmath127 are small ; the terms @xmath128 may be neglected in the numerator but should be retained in the denominator , so we get @xmath129 @xmath130 where we introduced a shorthand notation for the projectors @xmath131 and a new function @xmath132    multiplying both parts of  ( [ eq : bse_1 g ] ) by @xmath133 from the left and by @xmath134 from the right , after some manipulations with dirac algebra , we get @xmath135    in a moving system , a projection of the gluon momentum @xmath26 onto the direction of vector @xmath127 is @xmath27 , whereas all the other components are @xmath115 so we may assume that the former can be neglected ( it is a generalization of the instantaneous approximation in qcd ) .\n",
            "439\n",
            "439\n",
            "4332\n",
            "166\n",
            "abstract\n",
            "the problem of secret sharing over the gaussian wiretap channel is considered . \n",
            " a source and a destination intend to share secret information over a gaussian channel in the presence of a wiretapper who observes the transmission through another gaussian channel . \n",
            " two constraints are imposed on the source - to - destination channel ; namely , the source can transmit only binary phase shift keyed ( bpsk ) symbols , and symbol - by - symbol hard - decision quantization is applied to the received symbols of the destination . \n",
            " an error - free public channel is also available for the source and destination to exchange messages in order to help the secret sharing process . \n",
            " the wiretapper can perfectly observe all messages in the public channel . \n",
            " it is shown that a secret sharing scheme that employs a random ensemble of regular low density parity check ( ldpc ) codes can achieve the key capacity of the bpsk - constrained gaussian wiretap channel asymptotically with increasing block length . to accommodate practical constraints of finite block length and limited decoding complexity , fixed irregular ldpc codes \n",
            " are also designed to replace the regular ldpc code ensemble in the proposed secret sharing scheme .\n",
            "205\n",
            "10166\n",
            "Lex Rank Summary\n",
            "by setting @xmath41 to be the value of the bound   obtained as described ,  then @xmath154 will be considered a key - leakage rate pair achievable by @xmath89 .\n",
            "for the scheme of  @xcite  , the first ldpc code is set to be @xmath85 above ( i.e. , the rate-@xmath186 @xmath187-regular ldpc code ) .\n",
            "we are to design an irregular ldpc code @xmath85 and its subcode @xmath88 that work well for the channel from the ( quantized ) destination to source and the channel from the ( quantized ) destination to wiretapper , corresponding to the error probabilities @xmath184 and @xmath185 , respectively .\n",
            "to evaluate the performance of the proposed secret sharing scheme  , we employed an upper bound on the leakage information rate that depends on the decoding error probabilities of the decoder at the source and of a fictitious decoder at the wiretapper , which observes the wiretapper received sequence , the syndrome in the public channel as well as the secret key .\n",
            "as a result , this established that the key capacity of the bpsk - constrained gaussian wiretap channel can be achieved by employing the secret sharing regular ldpc code ensemble in the proposed scheme .\n",
            "199\n",
            "199\n",
            "10166\n",
            "205\n",
            "abstract\n",
            "in this paper , we report high - precision absolute distance and vibration measurements performed with frequency scanned interferometry using a pair of single - mode optical fibers . \n",
            " absolute distance was determined by counting the interference fringes produced while scanning the laser frequency . \n",
            " a high - finesse fabry - perot interferometer was used to determine frequency changes during scanning . \n",
            " two multiple - distance - measurement analysis techniques were developed to improve distance precision and to extract the amplitude and frequency of vibrations . under laboratory conditions , \n",
            " measurement precision of @xmath0 50 nm was achieved for absolute distances ranging from 0.1 meters to 0.7 meters by using the first multiple - distance - measurement technique . \n",
            " the second analysis technique has the capability to measure vibration frequencies ranging from 0.1 hz to 100 hz with amplitude as small as a few nanometers , without a _ priori _ knowledge . a possible optical alignment system for a silicon tracker is also presented .\n",
            "166\n",
            "2715\n",
            "Lex Rank Summary\n",
            "for a fsi system , drifts and vibrations occurring along the optical path during the scan will be magnified by a factor of @xmath21 , where @xmath11 is the average optical frequency of the laser beam and @xmath22 is the scanned frequency range .\n",
            "in order to extract the amplitude and frequency of the vibration , another multiple - distance - measurement technique called slip measurement window with fixed start point  is used , as shown in fig.2 .\n",
            "the rms of measured distances for 10 sequential scans is 1.6 @xmath1 if there is only one distance measurement per scan ( @xmath40 ) .\n",
            "two fsi demonstration systems , air fsi and optical fiber fsi , are constructed for extensive tests of multiple - distance - measurement technique , air fsi means fsi with the laser beam transported entirely in the ambient atmosphere , optical fiber fsi represents fsi with the laser beam delivered to the interferometer and received back by single - mode optical fibers .\n",
            "for the first laser , the measured distance @xmath46 , and @xmath47 is drift error during the laser scanning .\n",
            "183\n",
            "183\n",
            "2715\n",
            "166\n",
            "abstract\n",
            "we consider the extended 2d @xmath0 model at zero temperature . parameters of the model corresponds to doping by holes . using the low doping effective action \n",
            " we demonstrate that the system can 1 ) preserve the long range collinear antiferromagnetic order , 2 ) lead to a spin spiral state ( static or dynamic ) , 3 ) lead to the phase separation instability . \n",
            " we show that at parameters of the effective action corresponding to the single layer cuprate la@xmath1sr@xmath2cuo@xmath3 the spin spiral ground state is realized . \n",
            " we derive properties of magnetic excitations and calculate quantum fluctuations . quantum fluctuations \n",
            " destroy the static spin spiral at the critical doping @xmath4 . \n",
            " this is the point of the quantum phase transition to the spin - liquid state ( dynamic spin spiral ) . \n",
            " the state is still double degenerate with respect to the direction of the dynamic spiral , so this is a `` directional nematic '' . \n",
            " the superconducting pairing exists throughout the phase diagram and is not sensitive to the quantum phase transition . \n",
            " we also compare the calculated neutron scattering spectra with experimental data .\n",
            "190\n",
            "8503\n",
            "Lex Rank Summary\n",
            "@xcite .\n",
            "calculation of energy and its minimization with respect to @xmath122 gives the following value @xmath123 the ground state energy of the spiral state is below that of the nel state only if @xmath108 .\n",
            "( [ oq ] ) as for the nel state , but the magnon - holon vertex is smaller than ( [ vn ] ) by the factor @xmath129 , @xmath130 \\right\\ } \\ .\\end{aligned}\\ ] ] a calculation similar to that performed in section [ sec : neel ] for the nel state gives the following green s function for the field @xmath131 that describes the in - plane magnon @xmath132 where @xmath133 is given by eq .\n",
            "due to in - plane and out - of plane quantum fluctuations the static component of the staggered field @xmath58 is reduced , @xmath198 expectation values @xmath199 and @xmath200 can be expressed in terms of green s function or in terms of q - integrated spectral densities @xmath201 these expressions must be renormalized by subtraction of the ultraviolet - divergent contribution that corresponds to the undoped @xmath61-model .\n",
            "the spin wave pseudogap is opened in the spin - liquid phase , the q - integrated spectral density in this case is shown in fig.\n",
            "205\n",
            "205\n",
            "8503\n",
            "190\n",
            "abstract\n",
            "black strings , one class of higher dimensional analogues of black holes , were shown to be unstable to long wavelength perturbations by gregory and laflamme in 1992 , via a linear analysis . \n",
            " we revisit the problem through numerical solution of the full equations of motion , and focus on trying to determine the end - state of a perturbed , unstable black string . \n",
            " our preliminary results show that such a spacetime tends towards a solution resembling a sequence of spherical black holes connected by thin black strings , at least at intermediate times . \n",
            " however , our code fails then , primarily due to large gradients that develop in metric functions , as the coordinate system we use is not well adapted to the nature of the unfolding solution . \n",
            " we are thus unable to determine how close the solution we see is to the final end - state , though we do observe rich dynamical behavior of the system in the intermediate stages .\n",
            "168\n",
            "8283\n",
            "Lex Rank Summary\n",
            "all metric components defined via ( [ metric ] ) depend upon @xmath5 : @xmath6 is a time - like coordinate , @xmath7 is a radial coordinate , and @xmath8 is the coordinate along the length of the string .\n",
            "such an approximation can be obtained by looking for the boundary of the causal past of some @xmath73 surface that is sufficiently far outside the apparent horizon that it is certain not to be inside the event horizon , yet close enough to the apparent horizon that its causal past , tracing backwards from the end - time of the simulation , probes the region of interest of the spacetime .\n",
            "in particular , @xmath71 , as defined by  ( [ i ] ) evaluates to @xmath74 for the unperturbed black string solution , and as @xmath75 is an invariant in spherical symmetry ( i.e. it is proportional to the area of an @xmath73 2-sphere ) , we can compare @xmath76 to the values of @xmath71 computed from a numerical solution to get some indication of how close the computed solution is to a black string spacetime .\n",
            "[ i_ah_1000 ] we plot the normalized quantity @xmath114 evaluated on the apparent horizon of our numerical solution of the unstable spacetime@xmath115 is @xmath116 for a black string , and @xmath117 for a black hole .\n",
            "we restrict our search to simply connected apparent horizons that are periodic in z. such an apparent horizon can be described by a curve in the @xmath161 plane , which we define to be the level surface @xmath162 of the function @xmath163 in other words , the apparent horizon will be given by the curve @xmath164 .\n",
            "277\n",
            "277\n",
            "8283\n",
            "168\n",
            "abstract\n",
            "we present high - resolution echelle spectra of [ ] @xmath0 m emission from the classical t tauri star ( ctts ) tw hya obtained with michelle on gemini north . \n",
            " the line is centered at the stellar radial velocity and has an intrinsic fwhm of @xmath1 . \n",
            " the line width is broader than other narrow emission lines typically associated with the disk around tw hya . \n",
            " if formed in a disk , the line broadening could result from turbulence in a warm disk atmosphere , keplerian rotation at an average distance of 0.1 au from the star , or a photoevaporative flow from the optically - thin region of the disk . \n",
            " we place upper limits on the [ ] emission flux from the cttss dp tau and bp tau .\n",
            "132\n",
            "6104\n",
            "Lex Rank Summary\n",
            "we measure equivalent widths for the [ ] fine - structure line ( @xmath26  @xmath27 ) at @xmath28 @xmath7 m @xcite of @xmath29   for tw hya and @xmath30 upper limits of @xmath31 and @xmath32   for non - detections from bp tau and dp tau , respectively .\n",
            "with a combination of keplerian rotation and turbulence  , the line could form at disk radii larger than @xmath67 au and in gas cooler than @xmath69 k. alternatively , the width of the [ ] line could also be explained if the emission arises from a photoevaporative flow from the optically thin region of the disk ( at @xmath70 au ) .\n",
            "since  both the @xmath123 k fuv lines and @xmath124 k x - ray lines are attributed to the accretion flow @xcite , this estimated euv emission likely applies to emission produced near the accretion shock .\n",
            "however , models of euv or x - ray irradiated disks may explain some [ ] emission in the low - velocity components of cttss @xcite .\n",
            "that the [ ] lines are narrower than the [ ] line suggests that , if the [ ] emission is produced in a disk , it traces less turbulent gas or gas at larger disk radius than the [ ] emission .\n",
            "211\n",
            "211\n",
            "6104\n",
            "132\n",
            "abstract\n",
            "the use of radioactive beams opens a new frontier for fusion studies . \n",
            " the coupling to the continuum can be explored with very loosely bound nuclei . \n",
            " experiments were performed with beams of nuclei at or near the proton and neutron drip - lines to measure fusion and associated reactions in the vicinity of the coulomb barrier . \n",
            " in addition , the fusion yield is predicted to be enhanced in reactions involving very neutron - rich unstable nuclei . \n",
            " experimental measurements were carried out to investigate if it is feasible to use such beams to produce new heavy elements . \n",
            " the current status of these experimental activities is given in this review .\n",
            "113\n",
            "13264\n",
            "Lex Rank Summary\n",
            "the r.m.s .\n",
            "@xcite results of fusion measurements performed with some low intensity neutron - rich radioactive beams will be discussed in this paper .\n",
            "measurements of fusion of @xmath10f and @xmath23pb was performed with the radioactive @xmath10f produced by an in - flight method using the @xmath71(@xmath10o,@xmath10f)@xmath54 reaction at atlas.\n",
            "the ratio of @xmath10f to @xmath10o varied with beam energies but was usually around 1 . since the energy of the @xmath10o contaminant was approximately 20% lower than that of @xmath10f , the fusion of @xmath10o with the target  was estimated to contribute less than 3% to the total fusion cross section .\n",
            "it is noted that for the following systems involving neutron - rich ribs the excitation functions will be compared in reduced coordinates using the bass model fusion barrier@xcite , and @xmath75r@xmath25 with r=1.2(a@xmath27+a@xmath28 ) , where a@xmath17 and a@xmath24 are the mass of the projectile and target , respectively , to normalize the center - of - mass reaction energy and the cross section .\n",
            "165\n",
            "165\n",
            "13264\n",
            "113\n",
            "abstract\n",
            "a theory is developed to describe the effect of an intrinsic localized mode ( ilm ) on small vibrations in a monatomic chain with hard quartic anharmonicity . \n",
            " one prediction is the appearance in the chain of linear local modes nearby the ilm . to check this result , \n",
            " md calculations of vibrations under strong local excitation are carried through with high precision . \n",
            " the results fully confirm the prediction .\n",
            "71\n",
            "3358\n",
            "Lex Rank Summary\n",
            "this   follows  from  the  fact  that  these  terms  oscillate  in  time  with  the frequencies  @xmath42  and  @xmath43  ( here @xmath44 is the frequency of a small vibration ) , one of which , @xmath45 may be comparable with the perturbation @xmath31 .\n",
            "the parametric resonance parameter @xmath64 , which determines the frequency correction equals @xmath65    analytical calculations of odd and even llms for a lattice containing an even ilm with a range of nonlinear parameter @xmath57 values .\n",
            "given are the relative ilm frequency @xmath66 , the ilm amplitudes of the four next - to central particles @xmath12 with @xmath67 , the relative frequency of the odd and even llm @xmath68 and @xmath69 , the amplitudes of these modes @xmath70 and @xmath71 ( @xmath72 ) ; @xmath73 ; @xmath74 ( the frequencies of the odd llms are corrected for the time oscillatory perturbation ; @xmath64 and @xmath75 are the corresponding parameters of this perturbation . )\n",
            "when small additional amplitude shifts appropriate to the odd or even symmetry llm presented in table 1 are added to the ilm amplitude pattern , then additional small  peaks  appear   in  the  power  spectrum ,  one  at @xmath94 , and an even smaller symmetrically situated peak at @xmath95 .\n",
            "one is that an ilm introduces a periodically time - dependent perturbation that supports nonlinear mixing processes between the ilm and the llms and a second is that for a moving ilm the `` effective defect space '' with its associated llms will travel together with the nonlinear excitation .\n",
            "251\n",
            "251\n",
            "3358\n",
            "71\n",
            "abstract\n",
            "we develop a new notion of security against timing attacks where the attacker is able to simultaneously observe the execution time of a program and the probability of the values of low variables . \n",
            " we then show how to measure the security of a program with respect to this notion via a computable estimate of the timing leakage and use this estimate for cost optimisation .\n",
            "66\n",
            "10335\n",
            "Lex Rank Summary\n",
            "we develop a new notion of security against timing attacks where the attacker is able to simultaneously observe the execution time of a ( probabilistic ) program and the probability of the values of low variables .\n",
            "we introduce a general model for the semantics of programs where time and probability are explicitly introduced in order to keep track of both the probabilistic evolution of the program / system state and its running time .\n",
            "the execution model of programs which we will use in the following is that of a labelled transition system ; more precisely , we will consider probabilistic transition systems ( pts ) .\n",
            "in our example  we assume that the states depicted as @xmath64 and @xmath65 form two classes which the attacker can identify ( e.g. because @xmath64 and @xmath65 states have the same values for low , variables ) .\n",
            "if we compute the @xmath184 and @xmath191 values between all the pairs of systems we get the following results : @xmath206 from this we see that @xmath184 and @xmath191 are symmetric , i.e. the difference between two systems is symmetric ; that every system is bisimilar with itself , i.e. @xmath207 ( as we have an empty diagonal ) ; and that the difference between two systems is between zero and one with values in between very well possible .\n",
            "222\n",
            "222\n",
            "10335\n",
            "66\n",
            "abstract\n",
            "competition for available resources is natural amongst coexisting species , and the fittest contenders dominate over the rest in evolution . \n",
            " the dynamics of this selection is studied using a simple linear model . \n",
            " it has similarities to features of quantum computation , in particular conservation laws leading to destructive interference . \n",
            " compared to an altruistic scenario , competition introduces instability and eliminates the weaker species in a finite time .\n",
            "71\n",
            "2844\n",
            "Lex Rank Summary\n",
            "such a situation can be described by a set of linear evolution equations .\n",
            "to analyse the competitive stage , let us choose normalisations such that a unit population of any species consumes the same amount of resource , and the total resource available at any time is one .\n",
            "obviously , @xmath9 can be driven negative only if some @xmath6 is negative .\n",
            "the evolutionary behaviour depends on their signs : + ( a ) @xmath48 : the asymptotic population is proportional to @xmath32 .\n",
            "+ ( 3 ) evolution one by one eliminates species @xmath9 with some @xmath56 , till the reduced dimensional system no longer has any @xmath56 .\n",
            "108\n",
            "108\n",
            "2844\n",
            "71\n",
            "abstract\n",
            "the surface partition of large clusters is studied analytically within a frame - work of the `` hills and dales model '' . \n",
            " three formulations are solved exactly by using the laplace - fourier transformation method . in the limit of small amplitude deformations , the `` hills and dales model '' gives upper and lower bounds for the surface entropy coefficient of large clusters . \n",
            " a comparison with the 2- and 3-dimensional ising model surface entropy coefficients is made .\n",
            "81\n",
            "4369\n",
            "Lex Rank Summary\n",
            "the lower estimates for the surface entropy coefficients are found and compared to the corresponding 2- and 3-dimensional ising lattice values in sect .\n",
            "for the grand canonical surface partition ( gcsp )  the desired geometrical partition can be given in the excluded volume approximation @xcite as @xmath20 s_1^{-1 } } \\ , ,   % \\ ] ] where @xmath21 is the area occupied by the deformation of @xmath9-constituent base ( @xmath22 ) , @xmath23 is the full surface of the cluster , and @xmath24 is the @xmath6-dependent size of the maximal allowed base on the cluster .\n",
            "for finite amplitudes of deformations  this ensemble corresponds to the case of clusters of intermediate size , when its surface is sufficiently filled with deformations that it is impossible to add one more deformation of large base in order to conserve the cluster volume , but it is possible to place many deformations of a much smaller ( or even smallest ) base .\n",
            "then equations ( [ nsixteen ] ) and ( [ nseventeen ] ) , respectively become @xmath109 similar to the previous consideration , the leading term of the lower estimate for the surface partitions ( [ nfifteen ] ) is given by the real root @xmath110 of the system ( [ ntwfive ] ) and ( [ ntwsix ] ) @xmath111     shows the complex roots of the system of eqs .\n",
            "then we considered the limit of vanishing deformations for all three surface partitions , and obtained the upper and lower estimates for the surface entropy for each of these partitions .\n",
            "260\n",
            "260\n",
            "4369\n",
            "81\n",
            "abstract\n",
            "solvable supersymmetric algebraic model for descriptions of the spherical to @xmath0 shape - phase transition in even and odd mass nuclei is proposed . \n",
            " this model is based on dual algebraic structure and richardson - gaudin method , where the duality relations between the unitary and quasispin algebraic structures for the boson and fermion systems are extended to mixed boson - fermion system . \n",
            " the structure of two type of nuclear supersymmetry schemes , based on the u(6/2 ) and u(6/4 ) supergroups , is discussed . \n",
            " we investigate the change in level structure induced by the phase transition by doing a quantal analysis . by using the generalized quasispin algebra \n",
            " , it is shown that the nuclear supersymmetry concept can be also used for transitional regions in addition to dynamical symmetry limits . \n",
            " experimental evidence for the u(5)-o(6 ) transition in ru - rh and zn - cu supermultiplets is presented . \n",
            " the low - states energy spectra and b(e2)values for these nuclei have been calculated and compared with the experimental data .\n",
            "174\n",
            "6828\n",
            "Lex Rank Summary\n",
            "iachello @xcite extended the concept of critical symmetry to critical supersymmetry and provided a benchmark for the study of shape phase transition in odd - even nuclei and also j.jolie et al.@xcite studied qpts in odd - even nuclei using a supersymmetric approach in interacting boson - fermion model .\n",
            "(49)@xcite @xmath154    where @xmath155 is isoscalar factor and @xmath156 is a single - particle matrix element that is obtained as@xcite @xmath157 a test of supersymmetry is to see the extent to which the electric quadrupole transition probabilities of even - even and odd - a nuclei can be describe with the same coefficients of eq.\n",
            "according to the supersymmetry between bosons and fermions ,  the fermion is transformed into a boson , the system is described by the same set of parameters thus to achieve a better fit , states of both of even - even and odd - a nuclei were used .\n",
            "extracted values for effective charge parameters  have presented in table 3 .  tables.4(a , b , c , d ) show experimental and calculated values of b(e2 ) for negative parity states of rh and positive parity states of ru .\n",
            "new experimental data on the even - mass ruthenium and the odd - mass rhodium isotopes and zn - cu supermultiplets were used to test the predictions of the new supersymmetry scheme in dynamical symmetry limits and transition region and performed an analysis for these isotopes via a gqa - based hamiltonian .\n",
            "244\n",
            "244\n",
            "6828\n",
            "174\n",
            "abstract\n",
            "in this work , we propose a detailed computational framework for modelling the envelope of the swept volume , that is the boundary of the volume obtained by sweeping an input solid along a trajectory of rigid motions . our framework is adapted to the well - established industry - standard brep format to enable its implementation in modern cad systems . \n",
            " this is achieved via a `` local analysis '' , which covers parametrization and singularities , as well as a `` global theory '' which tackles face - boundaries , self - intersections and trim curves . \n",
            " central to the local analysis is the `` funnel '' which serves as a natural parameter space for the basic surfaces constituting the sweep . \n",
            " the trimming problem is reduced to the problem of surface - surface intersections of these basic surfaces . \n",
            " based on the complexity of these intersections , we introduce a novel classification of sweeps as either decomposable or non - decomposable . \n",
            " further , we construct an _ invariant _ function @xmath0 on the funnel which efficiently separates decomposable and non - decomposable sweeps . through a geometric theorem \n",
            " we also show intimate connections between @xmath0 , local curvatures and the inverse trajectory used in earlier works as an approach towards trimming . \n",
            " in contrast to the inverse trajectory approach , @xmath0 is robust and is the key to a complete structural understanding , and an efficient computation of both , the singular locus and the trim curves , which are central to a stable implementation . \n",
            " several illustrative outputs of a pilot implementation are included . \n",
            " sweeping , boundary representation , parametric curves and surfaces\n",
            "279\n",
            "11577\n",
            "Lex Rank Summary\n",
            "we also show that ( i ) singular trim curves make contact with the @xmath4 curves , and ( ii ) excision at the singular trim curves removes all singularities of the envelope except at these points of contact .\n",
            "note that @xmath171 is smooth if @xmath172 at all points in @xmath171 .\n",
            "further , let @xmath286 and @xmath287 be the envelope and contact - set for the sweeps @xmath284 respectively .\n",
            "@xmath688 and @xmath689 .\n",
            "@xmath703 and @xmath704 .\n",
            "76\n",
            "76\n",
            "11577\n",
            "279\n",
            "abstract\n",
            "thread - like structures are pervasive across scales , from polymeric proteins to root systems to galaxy filaments , and their characteristics can be readily investigated in the network formalism . yet , network links usually represent only parts of filaments , which , when neglected , may lead to erroneous conclusions from network - based analyses . the existing alternatives to detect filaments in network representations require tuning of parameters over a large range of values and treat all filaments equally , thus , precluding automated analysis of diverse filamentous systems . here , we propose a fully automated and robust optimisation - based approach to detect filaments of consistent intensities and angles in a given network . \n",
            " we test and demonstrate the accuracy of our solution with contrived , biological , and cosmic filamentous structures . \n",
            " in particular , we show that the proposed approach provides powerful automated means to study properties of individual actin filaments in their network context . \n",
            " our solution is made publicly available as an open - source tool , http://mathbiol.mpimp-golm.mpg.de/define/[define ] , facilitating decomposition of any given network into individual filaments . \n",
            " keywords : polymers , cytoskeleton , networks , path cover , computational complexity\n",
            "202\n",
            "19903\n",
            "Lex Rank Summary\n",
            "as an additional example , we study the all - to - all filament roughness @xmath23 which is the average maximal difference between any two edge weights in a filament @xmath20 , and again the original weight of the edge is used for a filament of length one .\n",
            "@xmath75 and @xmath76 ) .\n",
            "and z.n .\n",
            "and z.n .\n",
            "@xmath180 and @xmath181 ) .\n",
            "61\n",
            "61\n",
            "19903\n",
            "202\n",
            "abstract\n",
            "high - temperature expansions are presently the only viable approach to the numerical calculation of the higher susceptibilities for the spin and the scalar - field models on high - dimensional lattices \n",
            " . the critical amplitudes of these quantities enter into a sequence of universal amplitude - ratios which determine the critical equation of state . \n",
            " we have obtained a substantial extension through order 24 , of the high - temperature expansions of the free energy ( in presence of a magnetic field ) for the ising models with spin @xmath0 and for the lattice scalar field theory with quartic self - interaction , on the simple - cubic and the body - centered - cubic lattices in four , five and six spatial dimensions . a numerical analysis of the higher susceptibilities obtained from these expansions , yields results consistent with the widely accepted ideas , based on the renormalization group and the constructive approach to euclidean quantum field theory , concerning the no - interaction ( `` triviality '' ) property of the continuum ( scaling ) limit of spin-@xmath1 ising and lattice scalar - field models at and above the upper critical dimensionality .\n",
            "197\n",
            "10903\n",
            "Lex Rank Summary\n",
            "the quantities @xmath215 with @xmath225 , obtained by the unbiased method in the case of the the scalar - field model on the h5bcc and h6bcc lattices , for several values of the coupling @xmath226 , are plotted vs @xmath86 in fig.\n",
            "[isuimfh56bcc ] , we have reported our estimates for the ratios @xmath236 , @xmath237 , @xmath238 and @xmath239 vs the value @xmath1 of the spin for ising models on the h5bcc and h6bcc lattices .\n",
            "in complete agreement with the proven mf nature of the critical behavior , these ratios generally equal unity , within the accuracy expected from our approximations that , in this case , allows not only for the influence of the confluent corrections to scaling , but also for the uncertainties in the estimates of the critical temperatures needed to bias the calculations .\n",
            "rev d * 79 * , 105002 ( 2009 ) ; nucl .\n",
            "the dashed horizontal line represents the predicted value of the exponent of the logarithmic correction to the leading power behavior of the susceptibility.,width=3 ]     the exponent @xmath197 of the susceptibility vs the value @xmath1 of the spin , in the case of the spin-@xmath1 ising models on the h4sc , h4bcc , h5bcc and h6bcc lattices .\n",
            "206\n",
            "206\n",
            "10903\n",
            "197\n",
            "abstract\n",
            "extragalactic transient searches have historically been limited to looking for the _ appearance _ of new sources such as supernovae . \n",
            " it is now possible to carry out a new kind of survey that will do the opposite , that is , search for the _ disappearance _ of massive stars . \n",
            " this will entail the systematic observation of galaxies within a distance of 10 mpc in order to watch @xmath0 supergiants . \n",
            " reaching this critical number ensures that _ something _ will occur yearly , since these massive stars must end their lives with a core collapse within @xmath0 years . using deep imaging and image subtraction \n",
            " it is possible to determine the fates of these stars whether they end with a bang ( supernova ) or a whimper ( fall out of sight ) . \n",
            " such a survey would place completely new limits on the total rate of all core collapses , which is critical for determining the validity of supernova models . \n",
            " it would also determine the properties of supernova progenitors , better characterize poorly understood optical transients , such as @xmath1 carina - like mass ejections , find and characterize large numbers of cepheids , luminous blue variables and eclipsing binaries , and allow the discovery of any new phenomena that inhabit this relatively unexplored parameter space .\n",
            "222\n",
            "5625\n",
            "Lex Rank Summary\n",
            "in short  , the rate of bh formation could well be comparable to the rate of normal sne even for relatively low - mass progenitors .\n",
            "most studies of this scenario have focused on the collapse and its neutrino signature without examining the fate of the remainder of the stellar envelope ( e.g. , baumgarte et al . 1996 ; liebendrfer et al . 2004 ; sumiyoshi et al .  we are aware of no studies of the expected optical signatures for these scenarios .\n",
            "we estimate the relative core collapse sn rate of the galaxies using the results of cappellaro et al .  ( 1999 ) and then normalize the total rate to match that observed for these galaxies from 1970 - 2007 based on the sternberg astronomical institute sn catalogs ( see ando et al .  the resulting predicted and observed rates for the individual galaxies agree well , although the absolute , total normalization ranges from @xmath49/year for sne from 1970 - 2007 to @xmath50/year if we restrict ourselves to the `` modern '' era of robotic surveys ( 1997 - 2007 ) .\n",
            "[ fig : rate ] ) .\n",
            "finally , while we argue that we can now detect bh formation even if the signature is for a star to simply disappear , it would be very helpful to have more quantitative estimates of the optical signatures expected for the scenarios in figure  [ fig : outcomes ] .\n",
            "240\n",
            "240\n",
            "5625\n",
            "222\n",
            "abstract\n",
            "the correlations between multiplicities in two separated rapidity windows , is studied in the framework of the monte carlo model based on the picture of string formation in elementary collisions of colour dipoles . \n",
            " the hardness of the elementary collisions is defined by a transverse size of the interacting dipoles . \n",
            " the dependencies of the forward - backward correlation strength on the width and position of the pseudorapidity windows , as well as on transverse momentum range of observed particles were studied . \n",
            " it is demonstrated that taking into account of the string fusion effects improves the agreement with the available experimental data .\n",
            "104\n",
            "1426\n",
            "Lex Rank Summary\n",
            "experimentally , the multiplicity correlation coefficient , defined as @xmath0 , has been measured in a wide energy range @xcite as a function of pseudorapidity windows width , their position and transverse momentum region .\n",
            "namely the mean multiplicity @xmath3 and the mean transverse momentum @xmath4 of the particles produced from a cluster of @xmath5 overlapping strings are related to those ( @xmath6 ) from a single string : @xmath7{k } { p_t}_{1}.$ ] for realization of the string fusion prescription , we have used the discrete approach , in which a lattice with the cell area equal to the string transverse area @xmath8 is introduced .\n",
            "lines  the results of calculation in the model with and without string fusion , points  the experimental data @xcite.,scaledwidth=90.0% ]  figure [ fig : mv ] shows the dependence of the correlation coefficient on the width of the pseudorapidity windows at three energies .\n",
            "figure  [ fig:3 ] shows the dependence of @xmath18 on the @xmath22 at four energies , calculated in the monte carlo model , with a comparison to the experimental data @xcite .\n",
            "the forward - backward multiplicity correlation strength in pp collisions at high energy is studied in the monte carlo model with string formation and fusion .\n",
            "205\n",
            "205\n",
            "1426\n",
            "104\n",
            "abstract\n",
            "the sensitivity to the mass composition as well as the reconstruction of the energy of the primary particle are explored here by leveraging the features of the radio lateral distribution function . for the purpose of this analysis , a set of events measured with the lopes experiment \n",
            " is reproduced with the latest coreas radio simulation code . \n",
            " based on simulation predictions , a method which exploits the slope of the radio lateral distribution function is developed ( slope method ) and directly applied on measurements . as a result , the possibility to reconstruct both the energy and the x@xmath0 , i.e. depth of the shower maximum , of the cosmic ray air shower using radio data and achieving relatively small uncertainties is presented . \n",
            " radio detection , cosmic rays , air showers , lopes , xmax , primary energy 96.50.sd,95.55.jz\n",
            "142\n",
            "2586\n",
            "Lex Rank Summary\n",
            "on average ,  the primary energy is of @xmath1ev , the zenith angle is less than 40 degrees , and the maximum shower core distance is 90 m. + for each lopes measured event , one proton - generated air shower and one iron - generated air shower is produced with coreas @xcite ( qgsjet ii.03 is used as hadronic interaction model ) .\n",
            "for the purpose of this analysis ,  the simulations are created in order to reproduce a realistic case : on the one hand , information about the lopes selected events , such as core position , primary energy , and incoming direction reconstructed by kascade - grande are used as input parameters for the corsika showers @xcite .\n",
            "+ for the lopes simulated events a linear correlation with the reconstructed primary energy from kascade - grande is shown in fig.\n",
            "the radio amplitude at a specific distance from the shower axis , derived from the fit value at such distance , is correlated with the primary energy reconstructed by kascade - grande ( in fig.\n",
            "+     reconstructed with the slope method for the lopes measurements ( black ) and for coreas simulations ( proton ( dashed - blue ) and iron ( light - red ) ) of the same events , for the complete zenith angle range- 0 - 40 deg.,scaledwidth=140.0% ]    the x@xmath0 for lopes is reconstructed by using eq.\n",
            "232\n",
            "232\n",
            "2586\n",
            "142\n",
            "abstract\n",
            "a basic problem that confronts the standard cosmological models is the problem of initial singularity characterised by infinite material density , infinite temperature and infinite spacetime curvature . \n",
            " the inevitable existence of such a phase of the universe may be considered to be one of the major drawbacks of einstein s field equations . \n",
            " to some extent inflation models ameliorate this . in the present work we postulate that whenever matter ( radiation ) \n",
            " arises in flat spacetime , it introduces curvature and causes a repulsive interaction to develop . \n",
            " a modified energy momentum tensor is introduced towards this end , which invokes the temperature and entropy . \n",
            " this redefinition of the energy momentum distribution when applied to the early universe dynamics has the effect of producing a non - singular initial behaviour . \n",
            " the repulsive interaction introduces some features of an accelerating universe consistent with present observations of high redshift supernovae , etc .\n",
            "155\n",
            "4539\n",
            "Lex Rank Summary\n",
            "thus gravitational field equations in presence of matter could be written in the form @xmath1 @xmath0 is einstein tensor and @xmath2 is the tensor corresponding to repulsive interaction of spacetime .\n",
            "+ @xmath35 + in matter dominated era , @xmath36 and @xmath37 + [ assix ] 6 .  the hubble parameter at t = 0 is given by @xmath38^{1/2}\\ ] ] + here @xmath39 is the total density at t = 0 and it is given by @xmath40 + g is newtonian gravitational constant ` a ' is the radiation constant .\n",
            "in this paper  we hypothesize that introduction of matter is flat spacetime ( in the early universe ) , apart from causing a curvature ( given by einstein tensor ) would also give rise to another effect , i.e. , spacetime acquires a black body like temperature _ due to the curvature _ and becomes filled with radiation with a corresponding entropy density and a negative pressure leading to repulsive action making the spacetime to expand .\n",
            "the density parameter in the matter dominated era assumes the form @xmath152^{-1}\\ ] ] the present value of density parameter is obtained by putting @xmath153 we have @xmath154^{-1}\\ ] ] which is less than 1 , but very nearly equal to 1 .\n",
            "from the expression for density parameter in the radiation dominated era  it is clear that there is _ no flatness problem _ in this model .\n",
            "234\n",
            "234\n",
            "4539\n",
            "155\n",
            "abstract\n",
            "recent studies have found a positive correlation between the star - formation rate of galaxies and their gamma - ray luminosity . \n",
            " galaxies with a high star - formation rate are expected to produce a large amount of high - energy cosmic rays , which emit gamma - rays when interacting with the interstellar medium and radiation fields . \n",
            " we search for gamma - ray emission from a sample of galaxies within and beyond the local group with data from the lat instrument onboard the _ fermi _ satellite . \n",
            " we exclude recently detected galaxies ( ngc 253 , m82 , ngc 4945 , ngc 1068 , ngc 2146 , arp 220 ) and use seven years of cumulative `` pass 8 '' data from the lat in the 100 mev to 100 gev range . \n",
            " no new detections are seen in the data and upper limits for the gamma - ray fluxes are calculated . \n",
            " the correlation between gamma - ray luminosity and infrared luminosity for galaxies obtained using our new upper limits is in agreement with a previously published correlation , but the new upper limits imply that some galaxies are not as efficient gamma - ray emitters as previously thought . \n",
            " [ firstpage ]    galaxies : starburst  gamma - rays : galaxies cosmic rays\n",
            "217\n",
            "4800\n",
            "Lex Rank Summary\n",
            "the resulting source significance can be estimated as @xmath14 @xcite and therefore a tentative detection is made if the ts is greater than 25 .  results from the maximum likelihood analysis for each source are shown in table [ tab1 ] .\n",
            "we calculated an upper limit for ngc 3627 .  similarly , a maximum likelihood analysis for ngc 3079 ( a seyfert 2 galaxy ) , resulted in a ts value of 28 .  however , this galaxy is near the very bright source 3fgl j0957.6 + 5523 and such result can not be regarded as evidence for a detection .\n",
            "the source ngc 3079 is not seen above this energy and we calculate an upper limit on its flux above this energy and extrapolate the result above 100 mev to report the final upper limit .\n",
            "in order to obtain the best - fit relation between the gamma - ray and infrared luminosities with our data  , we applied a regression algorithm known as expectation - maximization , which is commonly used in survival analysis with censored data , such as those including upper limits , as implemented in the code asurv rev 1.2 @xcite .\n",
            "the scaling relation found here implies that for galaxies with sfr @xmath33 m@xmath34yr@xmath5 the maximum calorimetric efficiency is @xmath35% and for sfr @xmath36 m@xmath34yr@xmath5 , it is @xmath37% , which is at the lower end of some previously predicted values @xcite .\n",
            "236\n",
            "236\n",
            "4800\n",
            "217\n",
            "abstract\n",
            "let @xmath0 be an alexandrov space ( with curvature bounded below ) . \n",
            " we determine the maximal dimension of the isometry group @xmath1 of @xmath0 and show that @xmath0 is isometric to a riemannian manifold , provided the dimension of @xmath1 is maximal . \n",
            " we determine gaps in the possible dimensions of @xmath1 . \n",
            " we determine the maximal dimension of @xmath1 when the boundary @xmath2 is non - empty and classify up to homeomorphism alexandrov spaces with boundary and isometry group of maximal dimension . \n",
            " we also show that a symmetric alexandrov space is isometric to a riemannian manifold .\n",
            "100\n",
            "5996\n",
            "Lex Rank Summary\n",
            "it is enough to show that @xmath0 is isometric to a riemannian manifold , since the conclusion of the theorem holds in the riemannian case ( see , for instance , theorem 3.1 in @xcite , p. 46 ) .\n",
            "then @xmath1 contains no closed subgroups of dimension @xmath149 for @xmath150    let @xmath18 be a subgroup of dimension @xmath149 , and let @xmath20 be the isotropy group of @xmath29 at a regular point @xmath151 .\n",
            "using the fact that @xmath147 has no @xmath173-dimensional subgroups , it is easy to see that a @xmath176-dimensional alexandrov space @xmath0 with a group of isometries @xmath29 of dimension @xmath177 or @xmath172 must be a homogeneous space .\n",
            "then the isometry group @xmath1 contains no closed subgroup @xmath29 such that the dimension of @xmath29 falls into any of the ranges : + @xmath181    mann s arguments in @xcite carry over verbatim to our case , except for one detail : in cases a and b in the proof of theorem  1 in @xcite , one should choose the point @xmath182 to be regular and lying in a principal orbit ; this can be done , since the principal stratum is open and dense in @xmath0 and the set of regular points is dense in @xmath0 ( cf .\n",
            "it follows from the proof of theorem  [ t : dim_bound_bdry ] that , since the dimension of @xmath29 is maximal , the dimension of the orbit @xmath191 is @xmath184 and the dimension of the isotropy group @xmath20 is maximal .\n",
            "250\n",
            "250\n",
            "5996\n",
            "100\n",
            "abstract\n",
            "we experimentally investigate a double - pass parametric down - conversion scheme for producing pulsed , polarization - entangled photon pairs with high visibility . the amplitudes for creating photon pairs on each pass interfere to compensate for distinguishing characteristics that normally degrade two - photon visibility . \n",
            " the result is a high - flux source of polarization - entangled photon pulses that does not require spectral filtering . \n",
            " we observe quantum interference visibility of over 95% without the use of spectral filters for 200 femtosecond pulses , and up to 98.1% with 5 nm bandwidth filters .\n",
            "98\n",
            "5296\n",
            "Lex Rank Summary\n",
            "the polarization of the down - converted photons from the first pass is flipped ( h@xmath30v ) before they are reflected back into the crystal ( fig .\n",
            "@xcite .\n",
            "the visibility of the double - pass with 5 nm filters as a function of the coincidence count rate is shown in fig .\n",
            "this can be seen in the rl visibility of the individual passes in fig .\n",
            "( [ eq:2passbzero ] ) for @xmath58 .\n",
            "73\n",
            "73\n",
            "5296\n",
            "98\n",
            "abstract\n",
            "we study thermoelectric transport through a coherent molecular conductor connected to two electron and two phonon baths using the nonequilibrium green s function method . \n",
            " we focus on the mutual drag between electron and phonon transport as a result of ` momentum ' transfer , which happens only when there are at least two phonon degrees of freedom . after deriving expressions for the linear drag coefficients , obeying the onsager relation , we further investigate their effect on nonequilibrium transport . \n",
            " we show that the drag effect is closely related to two other phenomena : ( 1 ) adiabatic charge pumping through a coherent conductor ; ( 2 ) the current - induced nonconservative and effective magnetic forces on phonons .\n",
            "122\n",
            "6052\n",
            "Lex Rank Summary\n",
            "in this paper  , we study the nonequilibrium thermoelectric transport through a model device , connected to two electron and two phonon baths , including the e - ph interaction within the device .\n",
            "up to the 2nd order in @xmath17 , the result  is summarized as follows @xmath29 we define the positive current direction as that electrons / phonons go from the bath to the device , and @xmath30 , @xmath31 , @xmath32 are the electrical current , heat current carried by electrons and phonons , respectively .\n",
            "in this case , it is possible to extract heat from one of the phonon baths by applying a voltage bias , similar to a refrigerator , as shown in fig .\n",
            "that is , in eq .\n",
            "( [ eq : lang2 ] ) .\n",
            "131\n",
            "131\n",
            "6052\n",
            "122\n",
            "abstract\n",
            "we report the discovery using _ hubble space telescope _ imaging and keck spectroscopy of a very bright , highly magnified ( @xmath0 ) lyman break galaxy ( lbg ) at @xmath1 in the field of the massive @xmath2 cluster macsj2135.2@xmath30102 . \n",
            " the system comprises two high - surface brightness arcs with a maximum extent of @xmath4 , bracketing a central object which we identify as a massive early - type galaxy at @xmath5 . \n",
            " we construct a lens model which reproduces the main features of the system using a combination of a galaxy - scale lens and the foreground cluster . \n",
            " we show that the morphological , spectral and photometric properties of the arcs are consistent with them arising from the lensing of a single @xmath6 lbg . \n",
            " the most important feature of this system is that the lensing magnification results in an apparent magnitude of @xmath7 , making this one of the brightest lbgs known . \n",
            " such a high magnification provides the opportunity of obtaining very high signal to noise ( and potentially spatially resolved ) spectroscopy of a high redshift galaxy to study its physical properties . \n",
            " we present initial imaging and spectroscopy demonstrating the basic properties of the system and discuss the opportunities for future observations .\n",
            "211\n",
            "3384\n",
            "Lex Rank Summary\n",
            "in terms of our understanding of the internal properties of high redshift galaxies , the studies of the gravitationally lensed lyman break galaxy ( lbg ) cb58 by pettini et al .  ( 2000 , 2002 ) have demonstrated that high - signal - to - noise spectra of typical lbgs can be obtained with 10-m telescopes , if they are highly magnified as a result of being serendipitously positioned behind a suitable foreground gravitational lens .\n",
            "a search of the sdss dr4 shows that this object is well - detected with a total magnitude of @xmath23 , consistent with the _ hst _ measurement of @xmath24 for the light from both arcs , and @xmath25 , @xmath26 and @xmath27 for n , s and g1 respectively .\n",
            "however , a comparison of the spectra of the two arcs does show some marked differences : the profiles of the ly@xmath45 , ly@xmath53 and the stronger ism lines differ between n and s , and the continuum appears redder in s , indicating that n and s are images of different sources , either two galaxies , or more likely two regions within a single galaxy ( consistent with the lens reconstruction ) .\n",
            "in addition to this galaxy , we also serendipitously detect a further two galaxies which show [ oii]3727 at @xmath68 indicating the presence of a structure at this redshift .\n",
            "this very bright apparent magnitude results from gravitational lensing by a galaxy at @xmath5 and a cluster at @xmath2 which provide a combined magnification of @xmath99 .\n",
            "256\n",
            "256\n",
            "3384\n",
            "211\n",
            "abstract\n",
            "a model for the production of large rapidity gaps being implemented in the monte carlo event generator phojet is discussed . in this model , \n",
            " high - mass diffraction dissociation exhibits properties similar to hadron production in non - diffractive hadronic collisions at high energies . \n",
            " hard diffraction is described using leading - order qcd matrix elements together with a parton distribution function for the pomeron and pomeron - flux factorization . since this factorization \n",
            " is imposed on born graph level only , unitarity corrections lead to a non - factorizing flux function . \n",
            " rapidity gaps between jets are obtained by soft color reconnection . \n",
            " it was previously shown that this model is able to describe data on diffractive hadron production from the cern - sps collider and from the hera lepton - proton collider . in this work \n",
            " we focus on the model predictions for rapidity gap events in @xmath0@xmath0 collisions at @xmath1 gev and compare to tevatron data . \n",
            " # 1@xmath2#1    march 1998     +\n",
            "166\n",
            "4504\n",
            "Lex Rank Summary\n",
            "the pomeron is considered as a two - component object with the born graph cross section for pomeron exchange given by the sum of hard and soft cross sections .\n",
            "\\label{two - comp - diff0}\\ ] ] the diffractive eikonal functions read @xmath17 where @xmath18 is the parton model cross section for hard pomeron@xmath19 scattering ( @xmath19 can be a hadron , photon or pomeron ) .\n",
            "new in the present model is hard diffraction and multiple interactions in the diffractive hadron production , therefore we have again compared to this data and we find a reasonable agreement @xcite .\n",
            "the distributions are mass distributions in single and central diffraction ( fig .\n",
            "the ratio of @xmath64 at these energies calculated with phojet is consistent with the data , see fig .\n",
            "128\n",
            "128\n",
            "4504\n",
            "166\n",
            "abstract\n",
            "the stability of nonvolatile thin liquid films and of sessile droplets is strongly affected by finite size effects . \n",
            " we analyze their stability within the framework of density functional theory using the sharp kink approximation , i.e. , on the basis of an effective interface hamiltonian . \n",
            " we show that finite size effects suppress spinodal dewetting of films because it is driven by a long - wavelength instability \n",
            " . therefore nonvolatile films are stable if the substrate area is too small . \n",
            " similarly , nonvolatile droplets connected to a wetting film become unstable if the substrate area is too large . \n",
            " this instability of a nonvolatile sessile droplet turns out to be equivalent to the instability of a volatile drop which can atttain chemical equilibrium with its vapor .\n",
            "129\n",
            "10505\n",
            "Lex Rank Summary\n",
            "the height @xmath116 of the wetting film , the pressure @xmath59 , the disjoining pressure @xmath117 of the wetting film , and the ratio between the drop free energy @xmath118 and the free energy @xmath119 of a flat film with the same excess volume are shown in table  [ table ] for several values of @xmath120 .\n",
            "[ fig_dhf - laplace](a ) there is also a second branch of droplet solutions which are unstable and which have a pressure @xmath25 intermediate between the pressure of the metastable or stable droplets and of the flat film .\n",
            "as a function of the substrate size @xmath4 and of the excess volume @xmath120 for ( a ) @xmath177 and ( b ) @xmath178 , i.e. , for a fixed homogeneous film thickness @xmath179 and @xmath159 , respectively , and @xmath99 .\n",
            "@xmath247 denotes the volume of a film of thickness @xmath103 , @xmath245 is the minimal volume required to form a droplet , @xmath240 is the volume at which the free energies of the flat film and of the stable droplet are equal .\n",
            "[ maxwellfig ] the volume @xmath24 ( or excess volume @xmath344 ) at which the free energy of the flat film solution ( a film of homogeneous thickness @xmath306 ) equals the free energy of the stable droplet ( indicated by a thin vertical line in fig .\n",
            "225\n",
            "225\n",
            "10505\n",
            "129\n",
            "abstract\n",
            "we show that the two slit experiment in which a single quantum particle interferes with itself can be interpreted as a quantum fingerprinting protocol : the interference pattern exhibited by the particle contains information about the environment it encountered in the slits which would require much more communication to learn classically than is required quantum mechanically . \n",
            " an extension to the case where the particle has many internal degrees of freedom is suggested and its interpretation is discussed in detail . \n",
            " a possible experimental realization is proposed .\n",
            "88\n",
            "3647\n",
            "Lex Rank Summary\n",
            "in order to compare this with classical fingerprinting in the simultaneous message passing model , we suppose that alice can send one trit of classical information to the referee , whereas bob is limited and can only send one bit to the referee .\n",
            "on the other hand if the inputs are different , then the probability that the particle is in one of the @xmath54 states is at least @xmath55 .\n",
            "when alice and bob send the particle to the referee , the particle belongs to a hilbert space of dimension @xmath59 ( since there are @xmath41 paths from alice to the referee and @xmath41 paths from bob to the referee ) .\n",
            "in @xcite it is proven that in the simultaneous message passing model , if alice and bob have no shared randomness , if the referee uses a deterministic decision strategy , and if the error probability is less than @xmath78 , then the number @xmath79 of bits of communication sent by alice to the referee , and the number @xmath80 of bits of communication sent by bob to the referee , must obey @xmath81 .\n",
            "in fact it is not unreasonable to conjecture that non trivial quantum fingerprinting is possible for all values of @xmath11 , since we know that it is possible when @xmath94 ( particle with no internal degrees of freedom ) , and it is possible for sufficiently large @xmath95 .\n",
            "234\n",
            "234\n",
            "3647\n",
            "88\n",
            "abstract\n",
            "motivated by recent experiments in bose - einstein condensed atoms that have been confined in toroidal traps , we examine the stability of persistent currents in such systems . \n",
            " we investigate the extent that the stability of these currents may be tunable , and the possible difficulties in their creation and detection .\n",
            "53\n",
            "3818\n",
            "Lex Rank Summary\n",
            "in sec.iv we consider a periodic potential along the torus and examine the stability of persistent currents in such a potential .\n",
            "for example , for one unit of circulation that we consider here , the drift velocity is equal to @xmath25 .\n",
            "as a first application of our method , we consider a step - like potential of a fixed height ( equal to unity in our units ) along the torus , @xmath28 and investigate the critical value @xmath29 of the coupling @xmath27 that is necessary to maintain the stability of the current , as function of @xmath30 .\n",
            "the value of @xmath60 for the uniform case ( dashed line ) is also shown as a reference.,width=302,height=188 ]  in a previous study @xcite , we investigated the value of @xmath29 that is necessary to stabilize a current in the presence of a piecewise constant potential , with a randomly chosen amplitude .\n",
            "the value of @xmath60 for the uniform case ( dashed line ) is also shown as a reference.,width=302,height=188 ]  one question that needs to be investigated within the problems that we examine here is the effect of gravity on the stability of persistent currents .\n",
            "195\n",
            "195\n",
            "3818\n",
            "53\n",
            "abstract\n",
            "we present a low - energy effective model for the charge degrees of freedom in two - leg t - j ladders . starting from @xmath0 mean - field theory \n",
            " , we exclude the spin degrees of freedom which have an energy gap . at low temperatures , \n",
            " the mean - field solution is the staggered - flux phase . for gapless charge excitations \n",
            " the effective theory is the luther - emery liquid . \n",
            " our analysis is applicable at low doping and in the `` physical '' range of parameters @xmath1 where there is only one massless mode in the charge sector and no massless modes in the spin sector . within our model \n",
            " we make predictions about correlation exponents and the superconductivity order parameter , and discuss the comparison with the existing numerical results .\n",
            "136\n",
            "6943\n",
            "Lex Rank Summary\n",
            "the fluctuations about this mean - field state are described by gauge fields which have a gap , except for the in - phase fluctuations which form a 1 + 1-dimensional abelian gauge field .\n",
            "as a result  , we find that the low - energy effective theory consists of two degenerate bands of holons with a short - range interaction and coupled to a @xmath5 gauge - field .\n",
            "in this section we present the @xmath0 mean - field theory for the t - j hamiltonian @xmath10 on the ladder ( fig .\n",
            "using our slave - boson representation  , we express @xmath6 ( for nearest - neigbor @xmath8 and @xmath205 ) in terms of spinons and holons as @xmath208.\\ ] ] at low doping , the fermionic part of the correlation function ( 4.2 ) may be replaced by the mean - field order parameters @xmath209 and we find @xmath210 where @xmath202 and @xmath203 now denote the states in the holonic sector .\n",
            "( [ 2.6 ] )  ( [ 2.9 ] ) by @xmath224 and @xmath225 .\n",
            "176\n",
            "176\n",
            "6943\n",
            "136\n",
            "abstract\n",
            "the paradigm for agn unification is reviewed , in terms of its optical manifestation as obscuration in the equatorial plane and its radio manifestation as relativistic beaming of the jet emission . within this paradigm , observed agn properties depend strongly on orientation angle . \n",
            " the predictions of unification are commensurate with the local numbers of agn of various types . \n",
            " the outstanding question concerns a possible population of obscured agn at high redshift , which are thought to produce the x - ray background , although few are observed directly . \n",
            " we describe early results from the _ \n",
            " hst_-_sirtf_-_chandra _ goods survey , which has as one of its principal goals the search for such obscured agn . \n",
            " # 1_#1 _ # 1_#1 _ =    # 1 1.25 in .125 in .25 in\n",
            "134\n",
            "4538\n",
            "Lex Rank Summary\n",
            "a few luminous type  2 agn have been found at @xmath33 ( e.g. , stern et al .  2002 ; norman et al .  2002 ) , but certainly not as many as type  1 quasars found in optical / uv surveys at these redshifts .\n",
            "furthermore , this distinction is usually made in optical luminosity , which constitutes a highly variable fraction of the bolometric luminosity ( @xmath510% in type  1 agn , @xmath6% in type  2 agn ) .\n",
            "in a recent chandra survey of radio jets ,  sambruna et al . ( 2002 , 2003 ) showed that optical and x - ray emission from radio jets is common , and that for the higher redshift cases , it is well explained by a model in which relativistic electrons in the jet inverse - compton scatter infrared photons from the cosmic microwave background ( cmb ) .\n",
            "assuming the simplest plausible picture  that each radio - loud agn has a relativistic jet characterized by a single doppler factor ( one direction , one velocity ) , that each has a fixed fraction of total luminosity in intrinsic jet luminosity , and with a plausible distribution of lorentz factors among jets  it is straightforward to calculate the luminosity function that would be observed .\n",
            "such limits as are seen in the plots ( woo & urry 2002a ) are selection effects , either from the survey flux limit or from the steepness of the luminosity function ( high luminosities and/or high black hole masses are rare ) or from the likely mis - identification of agn as normal galaxies ( when the nucleus reaches low enough luminosity relative to the host galaxy ) .\n",
            "282\n",
            "282\n",
            "4538\n",
            "134\n",
            "abstract\n",
            "in this paper we discuss wild embeddings like alexanders horned ball and relate them to fractal spaces . we build a @xmath0-algebra corresponding to a wild embedding . \n",
            " we argue that a wild embedding is the result of a quantization process applied to a tame embedding . \n",
            " therefore quantum states are directly the wild embeddings . \n",
            " then we give an example of a wild embedding in the 4-dimensional spacetime . \n",
            " we discuss the consequences for cosmology .\n",
            "77\n",
            "6111\n",
            "Lex Rank Summary\n",
            "therefore the wild embedding ( alexanders horned ball ) can be seen as a quantization of a tame embedding , i.e. it is a quantum state .\n",
            "consider the wild embedding @xmath45 with @xmath46 and @xmath47 .\n",
            "finally we are able to define the @xmath3algebra associated to the wild embedding :    let @xmath90 be a wild embedding with @xmath91 as fundamental group of the complement @xmath92 .\n",
            "but for this example we will show that the enveloping von neumann algebra of this wild embedding ( alexanders horned ball ) is the result of a deformation quantization using the classical poisson algebra ( of closed curves ) of the tame embedding .\n",
            "but then , a wild embedding can be seen as a quantum state .\n",
            "121\n",
            "121\n",
            "6111\n",
            "77\n",
            "abstract\n",
            "we present results from our analysis of the near - infrared ( @xmath0 , @xmath1 , and @xmath2 ) photometry for all cataclysmic variables ( cvs ) from the catalog of @xcite that are detected in the ( final ) all sky data release ( asdr ) from the two micron all sky survey ( 2mass ) .\n",
            "58\n",
            "560\n",
            "Lex Rank Summary\n",
            "investigating cvs in the ir contributes to the understanding of system components that are expected to radiate at these wavelengths , such as the cool outer disk , accretion stream , and secondary star .\n",
            "the locations of another 376 cvs were securely identified , but these systems were too faint to be detected by 2mass .\n",
            "figure [ fig1 ] ( left ) shows the ir color - color diagram of all `` good '' cv detections from 2mass .\n",
            "the cvs located in outlying color regions ( e.g. , l dwarf region , lower right quadrant , etc . )\n",
            "we are currently updating the input target sample to include all cvs in @xcite up to 01 september 2004 for final analysis of the ir properties of cvs , to appear in a future publication .\n",
            "134\n",
            "134\n",
            "560\n",
            "58\n",
            "abstract\n",
            "in this paper we present some results of numerical simulations concerning the development of galactic winds in starburst galaxies . \n",
            " in particular , we focus on a galaxy similar to izw18 , the most metal - poor galaxy locally known . \n",
            " we compute the chemo - dynamical evolution of this galaxy , considering the energetic input and the chemical yields originating from supernovae ( sne ) of type ii and ia and from intermediate - mass stars . \n",
            " we consider both single , instantaneous starburst and two starburst separated by a quiescent period . in all considered cases a metal enriched wind develops and in particular the metals produced by type ia sne are ejected more efficiently than the other metals . \n",
            " we suggest that two bursts of star formation , the first being weaker and the last having an age of some tenth of myr , can satisfactorily reproduce the abundances and abundance ratios found in literature for izw18 . \n",
            " # 1_#1 _ # 1_#1 _ =    # 1 1.25 in .125 in .25 in\n",
            "176\n",
            "2210\n",
            "Lex Rank Summary\n",
            "both dynamical and chemical simulations of these galaxies have suggested the existence of a ` differential galactic wind ' , in the sense that , after a starburst event , these objects would loose mostly metals ( pilyugin 1992 , 1993 ; marconi , matteucci & tosi 1994 ; maclow & ferrara 1999 ; dercole & brighenti 1999 ) .\n",
            "the production of these elements are obtained following the nucleosynthesis prescriptions from various authors : woosley & weaver ( 1995 ) for sneii , nomoto , thielemann & yokoi for sneia and renzini & voli ( 1981 ) , case r , or van den hoek & groenewegen ( 1997 ) , case v , for ims .\n",
            "in the single - burst model , the mass of stars formed is @xmath5 m@xmath2 , whereas in the two - burst model we consider a weaker first burst ( the mass of stars is @xmath6 m@xmath2 ) .\n",
            "in particular ,  following results of bradamante , matteucci & dercole ( 1998 ) , we consider a thermalization efficiency of @xmath8 for the single - burst model and @xmath9 for the two - burst model , namely only 3% ( or 5% ) of the explosion energy is able to thermalize the ism , while the rest is radiated away .\n",
            "*  single - burst model reproduces the observed abundances in izw18 after @xmath14 31 myr , while for the two - burst model we obtain agreement with the data found in literature for wider ranges of time , when the second starburst has an age of some tenth of myr , depending on the adopted model and nucleosynthesis prescriptions .\n",
            "275\n",
            "275\n",
            "2210\n",
            "176\n",
            "abstract\n",
            "we propose an incentive scheme based on intervention to sustain cooperation among self - interested users . in the proposed scheme \n",
            " , an intervention device collects imperfect signals about the actions of the users for a test period , and then chooses the level of intervention that degrades the performance of the network for the remaining time period . \n",
            " we analyze the problems of designing an optimal intervention rule given a test period and choosing an optimal length of the test period . \n",
            " the intervention device can provide the incentive for cooperation by exerting intervention following signals that involve a high likelihood of deviation . \n",
            " increasing the length of the test period has two counteracting effects on the performance : it improves the quality of signals , but at the same time it weakens the incentive for cooperation due to increased delay .\n",
            "143\n",
            "3182\n",
            "Lex Rank Summary\n",
            "in an incentive scheme based on intervention  , a network is augmented with an intervention device that is able to monitor the actions of users and to take an action that affects the payoffs of users .\n",
            "in this paper , we consider a more realistic scenario where the intervention device can obtain only imperfect information about the actions of users and it takes time for the intervention device to collect signals .\n",
            "we consider a scenario where the intervention device collects signals from sensing the channel for the first @xmath14 slots , where @xmath15 , and then chooses its transmission probability , which can be interpreted as the intervention level .\n",
            "the expected payoff of user @xmath6 when the users choose action profile @xmath18 and the intervention device uses intervention rule @xmath29 can be expressed as @xmath33 a_i \\prod_{j \\in \\mathcal{n } \\setminus \\{i\\ } } ( 1-a_j).\\end{aligned}\\ ] ] note that @xmath34 can be interpreted as the expected transmission probability of the intervention device , while @xmath35 is the weight on the slots in which the action of the intervention device affects the users .\n",
            "then the lp problem has a feasible solution if and only if @xmath56 \\geq \\tau_d - \\tau_c.\\end{aligned}\\ ] ] moreover , if the lp problem has a feasible solution , then there exists a unique optimal solution @xmath48 described by @xmath57 \\right ] & \\textrm{if $ k=\\bar{k}$,}\\\\ 0 & \\textrm{if $ k>\\bar{k}$ , } \\end{array } \\right.\\end{aligned}\\ ] ] where @xmath58 \\geq \\tau_d - \\tau_c \\right\\}.\\end{aligned}\\ ] ]    define the likelihood ratio of signal @xmath25 ( i.e. , @xmath25 idle signals out of @xmath14 signals ) by @xmath59 it is easy to see that @xmath60 , @xmath61 , and @xmath62 is monotonically decreasing in @xmath25 .\n",
            "289\n",
            "289\n",
            "3182\n",
            "143\n",
            "abstract\n",
            "one of the unsolved issues in the quantum gravity comes from the wheeler - dewitt equation , which is the second order functional derivative equation with non - linear term . in this paper \n",
            " , we introduce a method to solve the wheeler - dewitt equation with the static restriction introduced in this paper . \n",
            " usually one treats the state functional of the spacetimes by the 3-dimensional metrics , which do not contain the timelike metrics . \n",
            " however we can expand this state to the state which has support on the space of the spacetime metrics with using additional constraint which requires the recovery of the 4-dimensional quantum gravity . enlarging the support of the state functional of the spacetime metrics \n",
            " , we can simply solve the usual wheeler - dewitt equation with the additional constraint . using this method \n",
            " we can solve some unsolved problems , such as the quantization of the black hole .\n",
            "156\n",
            "4694\n",
            "Lex Rank Summary\n",
            "first we add another dimension as an external time to the usual 4-dimensional metrics and create an enlarged hilbert space which has support of the spacetime metrics , and then we reduce this quantum state to the physical 4-dimensional state , we can obtain the additional constraint to simplify the usual wheeler - dewitt equation i.e. we use static restriction in a quantum gravity .\n",
            "_ in this method , in the @xmath33 additional constraint @xmath68 appears which we call static restriction , if there is no time evolution and the projection is defined by the definition 3 .\n",
            "@xmath124 from this equation we obtain @xmath125 or @xmath126 whose solution is @xmath127 from this result and eq .\n",
            "the modified 4 + 1 hamiltonian constraint is now written as @xmath132 while the usual 3 + 1 hamiltonian constraint is written as @xmath133 since finding a solution to ( [ 39 ] )  is something difficult , we use additional constraint @xmath134 to simplify it as @xmath135 both constraints @xmath129 and @xmath136 act on the state @xmath137 which belong to a subset of @xmath33 .\n",
            "from now on  there are no static restriction in the quantum gravity .\n",
            "193\n",
            "193\n",
            "4694\n",
            "156\n",
            "abstract\n",
            "we propose a conceptually novel method of reconstructing the topology of dynamical networks . by examining the correlation between the variable of one node and the derivative of another node \n",
            " , we derive a simple matrix equation yielding the network adjacency matrix . \n",
            " our assumptions are the possession of time series describing the network dynamics , and the precise knowledge of the interaction functions . \n",
            " our method involves a tunable parameter , allowing for the reconstruction precision to be optimized within the constraints of given dynamical data . \n",
            " the method is illustrated on a simple example , and the dependence of the reconstruction precision on the dynamical properties of time series is discussed . \n",
            " our theory is in principle applicable to any weighted or directed network whose internal interaction functions are known .    * \n",
            " derivative - variable correlation + reveals the structure of + dynamical networks * + zoran levnaji + _ faculty of information studies in novo mesto , + 8000 novo mesto , slovenia _ +\n",
            "168\n",
            "5619\n",
            "Lex Rank Summary\n",
            "[eq-4 ] from time @xmath42 to @xmath43 .\n",
            "this shows that besides the length and resolution of the time series , the reconstruction precision crucially depends on the `` quality '' of the time series as well , i.e. on the quantity of network information contained in them .\n",
            "however , the final reconstruction precision depends on a number of factors : ( _ i _ ) length and resolution of the time series , also related to the precision of derivative estimates ; ( _ ii _ ) quantity of network information contained in the empirical data , which can be seen as the reproducibility of time series , or coverage of the dynamical phase space with data ; ( _ iii _ ) noise in the systems , which can manifest itself either as an error in the measurement of @xmath3 or imprecision in the knowledge of @xmath11 and @xmath12 ; ( _ iv _ ) invertibility of the matrix @xmath55 , which becomes unstable for @xmath56 ( very important for larger networks ) ; and finally , ( _ v _ ) properties of the network itself  some networks are more reconstructable than others , due to exhibiting qualitatively different collective dynamics .\n",
            "we presented a novel method of reconstructing the topology of a general dynamical network from the time series and knowledge of interaction functions .\n",
            "and @xmath68 as function of the time series length @xmath4 , computed for the time series from fig.\n",
            "244\n",
            "244\n",
            "5619\n",
            "168\n",
            "abstract\n",
            "we provide a ` user guide ' to the literature of the past twenty years concerning the modeling and approximation of discontinuous solutions to nonlinear hyperbolic systems that admit _ small - scale dependent _ shock waves . \n",
            " we cover several classes of problems and solutions : nonclassical undercompressive shocks , hyperbolic systems in nonconservative form , boundary layer problems . \n",
            " we review the relevant models arising in continuum physics and describe the numerical methods that have been proposed to capture small - scale dependent solutions . in agreement with the general well - posedness theory , \n",
            " small - scale dependent solutions are characterized by a _ kinetic relation , _ a _ family of paths , _ or an _ admissible boundary set . \n",
            " _ we provide a review of numerical methods ( front tracking schemes , finite difference schemes , finite volume schemes ) , which , at the discrete level , reproduce the effect of the physically - meaningful dissipation mechanisms of interest in the applications . an essential role is played by the _ equivalent equation _ associated with discrete schemes , which is found to be relevant even for solutions containing shock waves .    [ firstpage ]    1.cm\n",
            "203\n",
            "18237\n",
            "Lex Rank Summary\n",
            "such small - scale dependent shocks exist for a variety of problems of physical interest , for instance , those modeled by conservative hyperbolic systems with dispersive phenomena ( e.g.  with capillary effects ) and nonconservative hyperbolic systems ( e.g.  for two - phase fluid flows ) , as well as boundary layer problems ( e.g.  with viscosity terms ) .\n",
            "these criteria are based on the prescription of a _  kinetic relation _ for conservative hyperbolic systems , a _ family of paths _ for nonconservative hyperbolic systems , and an _ admissible boundary set _ for boundary value problems .\n",
            "furthermore , if some structural conditions on the numerical flux @xmath95 are assumed as in ( tadmor 1987 , 2003 ) , one can show that the scheme in the limit also satisfies a discrete version of the entropy inequality , that is , [ eq : efdm1 ] u(u_i ) + ( g_i+1/2(t ) - g_i-1/2(t ) ) 0 . here ,  the _ numerical entropy flux _  @xmath96 is consistent with the entropy flux @xmath97 in , in the sense that @xmath98 for all relevant @xmath93 .\n",
            "however , standard numerical schemes may not converge to the physical viscosity solution of the initial boundary value problem for a system of conservation laws .\n",
            "the resulting numerical scheme with numerical flux , has been termed as the _ cnd _ scheme ( correct numerical diffusion scheme ) and was shown by mishra and spinolo ( 2011 ) to be i ) entropy stable and ii ) its equivalent equation matched the underlying parabolic regularization of the conservation law .\n",
            "268\n",
            "268\n",
            "18237\n",
            "203\n",
            "abstract\n",
            "daily interactions naturally define social circles . \n",
            " individuals tend to be friends with the people they spend time with and they choose to spend time with their friends , inextricably entangling physical location and social relationships . as a result \n",
            " , it is possible to predict not only someone s location from their friends locations but also friendship from spatial and temporal co - occurrence . \n",
            " while several models have been developed to separately describe mobility and the evolution of social networks , there is a lack of studies coupling social interactions and mobility . in this work \n",
            " , we introduce a model that bridges this gap by explicitly considering the feedback of mobility on the formation of social ties . \n",
            " data coming from three online social networks ( twitter , gowalla and brightkite ) is used for validation . \n",
            " our model reproduces various topological and physical properties of the networks not captured by models uncoupling mobility and social interactions such as : i ) the total size of the connected components , ii ) the distance distribution between connected users , iii ) the dependence of the reciprocity on the distance , iv ) the variation of the social overlap and the clustering with the distance . besides numerical simulations \n",
            " , a mean - field approach is also used to study analytically the main statistical features of the networks generated by a simplified version of our model . \n",
            " the robustness of the results to changes in the model parameters is explored , finding that a balance between friend visits and long - range random connections is essential to reproduce the geographical features of the empirical networks .\n",
            "278\n",
            "5422\n",
            "Lex Rank Summary\n",
            "furthermore , it has been shown that online  @xcite social links can be inferred from user co - occurrences in space and time and , likewise , that the location of a person can be predicted from the geographic positions of his or her online friends  @xcite .\n",
            "some further aspects of the relation between geography and online social contacts have been studied such as the probability that a link at a given distance closes a triangle  @xcite , the connections between users in different countries  @xcite , the social interactions and mobility in emergency situations  @xcite or the overlap between users ego networks and how it decays with the distance  @xcite .\n",
            "[ cols=\"^,^,^,^,^,^,^,^,^ \" , ]     the geo - social properties of the networks generated by the tf model are shown in figure  5 for the us and in supplementary figures  [ supfig_3 ] and [ supfig_4 ] for the uk and germany , respectively .\n",
            "the error @xmath12 of this null model is between @xmath13-@xmath14 for the three countries , around twice the error of the tf model ( see figure  6 ) .\n",
            "our results show that by establishing an appropriate balance between friend visits and random link creation , the model can reproduce the main features of online social networks , e.g. , we show that @xmath58 of the mobility has to be directed towards existing friends .\n",
            "229\n",
            "229\n",
            "5422\n",
            "278\n",
            "abstract\n",
            "this study introduces a modified quadratic lorenz attractor . \n",
            " the properties of this new chaotic system are analysed and discussed in detail , by determining the equilibria points , the eigenvalues of the jacobian , and the lyapunov exponents . \n",
            " the numerical simulations , the time series analysis , and the projections to the @xmath0-plane , @xmath1-plane , and @xmath2-plane are conducted to highlight the chaotic behaviour . \n",
            " the multiplicative form of the new system is also presented and the simulations are conducted using multiplicative runge - kutta methods .\n",
            "90\n",
            "2155\n",
            "Lex Rank Summary\n",
            "the application areas of dynamical systems can be found e.g. in many disciplines in physics @xcite , population dynamics in biology @xcite , and chemical kinetics in chemistry @xcite .\n",
            "the study on `` the equation for continuous chaos '' by rssler @xcite can be seen as another landmark in the discussion of 3d dynamic systems .\n",
            "in order to determine the equilibrium points of the proposed system -  , we need to solve the system    @xmath18    thus , the solution of the system with respect to @xmath11 , @xmath12 , @xmath13 give the equilibria points as :    @xmath19{\\beta\\,\\rho^3},\\sqrt[4]{\\frac{\\beta}{\\rho}},\\rho\\right ) \\\\  \\it e^-&=&\\left(-\\sqrt[4]{\\beta\\,\\rho^3},-\\sqrt[4]{\\frac{\\beta}{\\rho}},\\rho\\right)\\end{aligned}\\ ] ]    for the parameters chosen in , the numerical values of the equilibria points are    @xmath20    in order to decide on the stability of the new proposed system , the eigenvalues of the jacobian matrix must be analyzed .\n",
            "by choosing the same values for the parameters , such as @xmath15 , @xmath16 with varying @xmath6 and the initial values as @xmath51  , we can see that the solutions of the geometric chaotic system and the bigeometric chaotic system will be similar to the ones that we get from the solutions of the chaotic system - .\n",
            "the following figure shows the chaotic behaviour of the geometric and the bigeometric dynamic systems when the parameters are chosen as @xmath15 , @xmath16 and @xmath52 .\n",
            "224\n",
            "224\n",
            "2155\n",
            "90\n",
            "abstract\n",
            "the 2df galaxy redshift survey ( 2dfgrs ) of 230,000 redshifts of nearby ( @xmath0 ) galaxies is now complete . \n",
            " it has allowed the 2dfgrs team and others to estimate fundamental cosmological parameters and to study galaxy intrinsic properties . here \n",
            " we highlight three recent key results from the survey : ( i ) an upper limit of about 2ev on the total mass of the three neutrino flavours , and an intriguing reasonable fitting of the 2dfgrs power spectrum to a mixed dark matter model without a cosmological constant , but with a low hubble constant ; ( ii ) the bimodality of the galaxy population in both spectral parameterisation and in colour ; and ( iii ) the clustering of different galaxy types and evidence for relative stochastic biasing . \n",
            " [ firstpage ]    dark matter - galaxies : clusters - galaxies :\n",
            "145\n",
            "2091\n",
            "Lex Rank Summary\n",
            "percival et al .  ( 2001 ) , efstathiou et al .  ( 2002 ) and lahav et al .  ( 2002 ) compared the 2dfgrs and cmb power spectra , and concluded that they are consistent with each other .\n",
            "for  fixed ` concordance model ' parameters @xmath17 , @xmath18 and a hubble constant @xmath19 , the amplitude of 2dfgrs galaxies in redshift space is @xmath20 ( at the survey s effective luminosity and redshift ) .\n",
            "recently the sdss team presented their results for the power spectrum ( tegmark et al .  2003a , b ; pope et al . 2004 ) , and they found good agreement with the 2dfgrs gross shape of the power spectrum .\n",
            "while it is established that the effect of neutrinos on the evolution of cosmic structure is small , the upper limits derived from large - scale structure could help significantly to constrain the absolute scale of the neutrino masses .\n",
            "it turns out that @xmath31 is a useful indicator of the star formation rate in a galaxy ( madgwick et al .  this allows us to divide the 2dfgrs into @xmath31-types , and to study e.g. luminosity functions and clustering per type .\n",
            "199\n",
            "199\n",
            "2091\n",
            "145\n",
            "abstract\n",
            "hydrogen and helium demix when sufficiently cool , and this bears on the evolution of all giant planets at large separations at or below roughly a jupiter mass . \n",
            " we model the thermal evolution of jupiter , including its evolving helium distribution following results of ab initio simulations for helium immiscibility in metallic hydrogen . after 4 gyr of homogeneous evolution \n",
            " , differentiation establishes a thin helium gradient below 1 mbar that dynamically stabilizes the fluid to convection . \n",
            " the region undergoes overstable double - diffusive convection ( oddc ) , whose weak heat transport maintains a superadiabatic temperature gradient . with a generic parameterization for the oddc efficiency , the models can reconcile jupiter s intrinsix flux , atmospheric helium content , and radius at the age of the solar system if the lorenzen et al . \n",
            " h - he phase diagram is translated to lower temperatures . \n",
            " we cast the evolutionary models in an mcmc framework to explore tens of thousands of evolutionary sequences , retrieving probability distributions for the total heavy element mass , the superadiabaticity of the temperature gradient due to oddc , and the phase diagram perturbation . \n",
            " the adopted scvh - iequation of state favors inefficient oddc such that a thermal boundary layer is formed , allowing the molecular envelope to cool rapidly while the deeper interior actually heats up over time . if the overall cooling time is modulated with an additional free parameter to imitate the effect of a colder or warmer eos , the models favor those that are colder than scvh - i . in this case \n",
            " the superadiabaticity is modest and a warming or cooling deep interior are equally likely .\n",
            "282\n",
            "10530\n",
            "Lex Rank Summary\n",
            "in this paper , we also allow for a global temperature offset @xmath8 to this phase diagram and estimate its value from available data ; we confirm the result of @xcite that for models computed with scvh - i , the necessary downward offset is of order 200 k. shifts to the published phase diagram in pressure are also conceivable , but as the phase diagrams of @xcite and @xcite agree fairly closely on the minimum _ pressure _ for phase separation at temperatures typical of jupiter and saturn s molecular - metallic transitions , the temperature offset appears to be the most important correction .\n",
            "assuming the microscopic diffusivity @xmath72 to be of order the he - he self - diffusion coefficient obtained in the recent _ ab initio _  simulations by @xcite , the timescale to form a sinkable droplet is @xmath73 the strong hierarchy in timescales @xmath74 implies that the transport of excess helium toward the center of the planet is probably efficient in spite of convection ( or double - diffusive convection , which mixes material over much longer timescales ) , so assuming the equilibrium mixture throughout the planet at each timestep is an adequate starting point for evolutionary models .\n",
            "since the phase diagram of @xcite provides the equilibrium helium abundance over @xmath2 space , and these are also the independent variables in the @xcite eos , we choose to adopt @xmath120 as the thermodynamic basis for our ` mesa`calculations .\n",
            "time for homogeneous @xmath153 models to cool to jupiter s @xmath3 as a function of their heavy - element mass @xmath6 and equilibrium temperature @xmath9 .\n",
            "of the temperature profile in the helium gradient region .\n",
            "279\n",
            "279\n",
            "10530\n",
            "282\n",
            "abstract\n",
            "recently , brodsky , hwang and schmidt have proposed a new mechanism that gives a transverse spin symmetry at leading twist in semi - inclusive deep - inelastic scattering . \n",
            " i show that the new mechanism is compatible with factorization and is due to an transverse - spin asymmetry in the @xmath0 distribution of quarks in a hadron ( the `` sivers asymmetry '' ) . \n",
            " an earlier proof that the sivers asymmetry vanishes because of time - reversal invariance is invalidated by the path - ordered exponential of the gluon field in the operator definition of parton densities . \n",
            " instead , the time - reversal argument shows that the sivers asymmetry is reversed in sign in hadron - induced hard processes ( e.g. , drell - yan ) , thereby violating naive universality of parton densities . \n",
            " previous phenomenology with time - reversal - odd parton densities is therefore validated .\n",
            "152\n",
            "4156\n",
            "Lex Rank Summary\n",
            "in this letter  , i will explore some important consequences of the results of bhs :    * it is completely consistent with factorization , and provides an existence proof of the sivers asymmetry @xcite , that is , of a transverse - spin - dependent azimuthal asymmetry of the distribution of quarks in a proton .\n",
            "since the momentum @xmath4 of the exchanged gluon is in a region associated with rescattering , the calculated ssa appears , at first sight , to be in contradiction with the factorization theorem , and its proof .\n",
            "the ssa in the cross section is therefore due to an ssa in the dependence of the parton density on transverse momentum .\n",
            "since , as we will see , the past - pointing wilson lines are appropriate for factorization in the drell - yan process , the correct result is not that the sivers asymmetry vanishes , but that it has opposite signs in dis and in drell - yan : @xmath18    in a sense ,  i have derived the situation suggested by anselmino , barone , drago and murgia @xcite , that non - standard time - reversal properties can enable the sivers asymmetry to exist .\n",
            "d * 43 * ( 1991 ) 261 .  collins , nucl .\n",
            "212\n",
            "212\n",
            "4156\n",
            "152\n",
            "abstract\n",
            "in this paper we describe in detail the implementation and main properties of a new inversion code for the polarized radiative transfer equation ( vfisv : very fast inversion of the stokes vector ) . \n",
            " vfisv will routinely analyze pipeline data from the helioseismic and magnetic imager ( hmi ) on - board of the solar dynamics observatory ( sdo ) . \n",
            " it will provide full - disk maps ( 4096@xmath04096 pixels ) of the magnetic field vector on the solar photosphere every 10 minutes . \n",
            " for this reason vfisv is optimized to achieve an inversion speed that will allow it to invert 16 million pixels every 10 minutes with a modest number ( approx . \n",
            " 50 ) of cpus . here \n",
            " we focus on describing a number of important details , simplifications and tweaks that have allowed us to significantly speed up the inversion process . \n",
            " we also give details on tests performed with data from the spectropolarimeter on - board of the hinode spacecraft . \n",
            " example.eps gsave newpath 20 20 moveto 20 220 lineto 220 220 lineto 220 20 lineto closepath 2 setlinewidth gsave .4 setgray fill grestore stroke grestore\n",
            "192\n",
            "3315\n",
            "Lex Rank Summary\n",
            "consequently , very fast ( _ 3000 - 10000 pixels / second _ ) inversion strategies such a principal component analysis ( pca ; rees et al .  2000 ; socas - navarro et al .  2001 ) or artificial neural networks ( anns ; socas - navarro 2003 , 2005 ) could meet the hmi requirements with a very small number of cpus .\n",
            "in section 6  we present a study of the inversion code s profile and speed .\n",
            "this fit is done by producing a synthetic stokes vector @xmath12 , that it is then compared at each wavelength position with the observed one via the @xmath6 of the fit :    @xmath13 ^ 2 \\frac{w_{ij}^2}{\\sigma_i^2}\\ ] ]    where @xmath14 is the number of wavelength points observed ( @xmath15 in hmi s case ) and @xmath16 is the number of free parameters .\n",
            "at this pace  it will be possible to provide solar full - disk maps ( with 1 \" resolution ) of the solar magnetic field vector every 10 minutes , using less than 40 cpus .\n",
            "& thorne , p. 1994 : apjs , 94 , 221 - 459 neckel , h. & labs , d. 1994 : _ solar phys _ , 153 , 91 - 114 landolfi , m. & landi deglinnocenti , e. 1982 : _ solar phys _ , 78 , 355 lites , b. , casini , r. , garcia , j.\n",
            "237\n",
            "237\n",
            "3315\n",
            "192\n",
            "abstract\n",
            "we propose an optical double - cavity resonator whose response to a signal is similar to that of an electromagnetically induced transparency ( eit ) medium . \n",
            " a combination of such a device with a four - level eit medium can serve for achieving large cross - kerr modulation of a probe field by a signal field . \n",
            " this would offer the possibility of building a quantum logic gate based on photonic qubits . \n",
            " we discuss the technical requirements that are necessary for realizing a probe - photon phase shift of @xmath0 caused by a single - photon signal . \n",
            " the main difficulty is the requirement of an ultra - low reflectivity beamsplitter and to operate a sufficiently dense cool eit medium in a cavity .\n",
            "126\n",
            "5922\n",
            "Lex Rank Summary\n",
            "in the free - medium regime , a probe pulse , which is desired to be influenced by a signal pulse , moves in a free eit medium and has thus a very small group velocity @xcite .\n",
            "the disadvantage of such a scheme is that most of the signal - photon energy is wasted dressing the atoms of the ( second ) eit medium @xcite and only small fraction @xmath5 of it is available for shifting the phase of the probe .\n",
            "the loss coefficient @xmath89 ( inverse absorption length ) for single - photon probe absorption can be given by @xcite @xmath90 where @xmath91 is the detuning of the probe from the transition , and @xmath92 is the decay rate of the state @xmath93 .\n",
            "the condition that then reads as @xmath115 and the condition of the two - photon absorption probability being much smaller than the phase shift ( [ dphires ] ) is @xmath116 which corresponds to the result in ref .\n",
            "( [ vg ] ) it then follows that this assumption yields the condition that @xmath118 by combining the conditions ( [ conddelta1 ] ) and ( [ conddelta2 ] ) , we obtain a condition for the atomic density , @xmath119 and a condition for the line - width of the probe , @xmath120    from eq .\n",
            "220\n",
            "220\n",
            "5922\n",
            "126\n",
            "abstract\n",
            "we have adopted the multistep shell model in the complex energy plane to study nuclear excitations occurring in the continuum part of the spectrum . in this method one \n",
            " proceeds by solving the shell model equations in a successive manner . \n",
            " that is , in each step one constructs the building blocks to be used in future steps . \n",
            " we applied this formalism to analyze the unbound nuclei @xmath0li starting from the one - particle states in @xmath1li and two - particle states in @xmath2li . in the former case \n",
            " the excitations correspond to the motion of three particles partitioned as the product of a one - particle and two - particle systems . \n",
            " the ground state of @xmath3li is thus calculated to be an antibound ( virtual ) state . in the four - particle system \n",
            " @xmath4li the states can be constructed as the coupling of two correlated pairs . \n",
            " we found that there is no bound or antibound state in @xmath4li .\n",
            "164\n",
            "3727\n",
            "Lex Rank Summary\n",
            "this formalism is an extension of the shell model in the complex energy plane  @xcite .\n",
            "one thus obtains @xmath72 the expression in the bracket is therefore the hermitian matrix @xmath45 , which can be written as @xmath73  using the berggren single - particle representation described above , we will evaluate the complex energies and wave functions of the unbound nuclei @xmath0li using the msm basis states consisting of the berggren one - particular states , which are states in @xmath1li , times the two - particle states corresponding to @xmath2li .\n",
            "by using single - particle energies ( i.e. , states in @xmath1li ) as provided by experimental data when available or as provided by our calculation  , we found that the only physically meaningful two - particle states are @xmath2li(gs ) , which is a bound state , and @xmath2li(@xmath89 ) , which is a resonance .\n",
            "that the ground state is an antibound ( or virtual )  state was confirmed by a number of experiments @xcite and the state @xmath93 has probably been observed in @xcite .\n",
            "623 - 2009 - 7340 and 2010 - 4723 .\n",
            "186\n",
            "186\n",
            "3727\n",
            "164\n",
            "abstract\n",
            "we analyzed temporal and spectral properties , focusing on the short bursts , for three anomalous x - ray pulsars ( axps ) and soft gamma repeaters ( sgrs ) , including , and . using the data from _ xmm - newton _ , we located the short bursts by bayesian blocks algorithm . \n",
            " the short bursts duration distributions for three sources were fitted by two lognormal functions . \n",
            " the spectra of shorter bursts ( @xmath0 ) and longer bursts ( @xmath1 ) can be well fitted in two blackbody components model or optically thin thermal bremsstrahlung model for . \n",
            " we also found that there is a positive correlation between the burst luminosity and the persistent luminosity with a power law index @xmath2 . \n",
            " the energy ratio of this persistent emission to the time averaged short bursts is in the range of @xmath3 , being comparable to the case in type x - ray burst .\n",
            "157\n",
            "6710\n",
            "Lex Rank Summary\n",
            "in order to compute the flux and luminosity  , we fitted the persistent spectrum for each observation and burst spectra for the observations with more than 50 burst photons .\n",
            "to investigate the spectral properties of short time scale bursts and long time scale bursts  , we divided the bursts into two subclasses at 0.2 s for , since has enough burst photons for spectral fitting and @xmath72 is the approximate intersecting point of these two components .\n",
            "this model is also widely used in the burst spectra fitting in axps / sgrs , but it is not always effective @xcite .\n",
            "both the persistent emission and the bursts are from the magnetic energy .\n",
            "in type  x - ray bursts , the energy ratio can be calculated for each burst , while in axps / sgrs , this ratio can only be analyzed for a long period with many bursts .\n",
            "148\n",
            "148\n",
            "6710\n",
            "157\n",
            "abstract\n",
            "all - dielectric `` magnetic light '' nanophotonics based on high refractive index nanoparticles allows controlling magnetic component of light at nanoscale without having high dissipative losses . \n",
            " the artificial magnetic optical response of such nanoparticles originates from circular displacement currents excited inside those structures and strongly depends on geometry and dispersion of optical materials . here a new approach for increasing magnetic response via resonant bianisotropy effect is proposed and analyzed . \n",
            " the key mechanism of enhancement is based on electric - magnetic interaction between two electrically and magnetically resonant nanoparticles of all - dielectric dimer nanoantenna . \n",
            " it was shown that proper geometrical arrangement of the dimer in respect to the incident illumination direction allows flexible control over all vectorial components of magnetic polarizability , tailoring the later in the dynamical range of 100@xmath0 and enhancement up to 36@xmath0 relative to performances of standalone spherical particles . \n",
            " the proposed approach provides pathways for designs of all - dielectric metamaterials and metasurfaces with strong magnetic response .\n",
            "168\n",
            "3323\n",
            "Lex Rank Summary\n",
            "the electric and magnetic polarizabilities which are associated with induced electric and magnetic moments have been also calculated ( fig .\n",
            "electric dipolar resonance of 70-nm radius particle overlaps with the magnetic dipolar resonance of 52-nm sphere at @xmath8 nm.,scaledwidth=50.0% ]    next , the scattering of a plane wave on all - dielectric dimer nanoantenna will be analyzed .\n",
            "following the cemda method , total electromagnetic fields [ both electric ( @xmath9 ) and magnetic ( @xmath10 ) ] were decomposed into incident and scattered components : @xmath11 where indices @xmath12 denote first ( bigger ) and second ( smaller ) nanoparticles , respectively , @xmath13 and @xmath14 are electric and magnetic fields of the incident plane wave , @xmath15 and @xmath16 are the full electric and magnetic fields at the position of the first ( electric ) nanoparticle ( with radius - vector @xmath17 ) , @xmath18 and @xmath19 are the electric and magnetic fields scattered by the second ( smaller ) nanoparticle at the first particle center , and analogously for the second particle .\n",
            "both particles are polarized by the incident field , as well as by the scattered one : @xmath20 where @xmath21 and @xmath22 are the electric and magnetic polarizabilities of single particle @xmath23 : @xmath24 and @xmath25 is the dielectric constant , @xmath26 is the imaginary unit .\n",
            "while standalone nanoparticles allow obtaining dipolar and high - multipolar resonant responses at the desired wavelength in the visible range specifying their radii and materials , a system of two coupled nanoparticles possesses more degrees of freedom .\n",
            "258\n",
            "258\n",
            "3323\n",
            "168\n",
            "abstract\n",
            "most models of dark energy predict the beginning of the accelerated epoch at @xmath0 . however , there are no observational or theoretical evidences in favor of such a recent start of the cosmic acceleration . \n",
            " in fact , a model of dark energy coupled to dark matter is explicitely constructed that _ a _ ) is accelerated even at high @xmath1 ; _ b _ ) allows structure formation during acceleration ; and _ c _ ) is consistent with the type ia supernovae hubble diagram , including the farthest known supernova sn1997ff at @xmath2 . \n",
            " it is shown that the accelerated epoch in this model could have started as early as @xmath3 . \n",
            " [ firstpage ]\n",
            "118\n",
            "4402\n",
            "Lex Rank Summary\n",
            "however , the nature of the dark energy is still enigmatic ( wetterich 1988 ; ratra & peebles 1988 ; frieman et al . 1995 ; caldwell et al .  its equation of state and its interaction with dark matter are in fact so far subject only to very weak constraints ( perlmutter et al .  1999 , huey et al . 1999 ,  baccigalupi et al .  2002 , corasaniti & copeland 2002 , bean & melchiorri 2002 , amendola et al .  2002 ) so that there exist a large variety of different dark energy models still viable ( see for instance the review by peebles & ratra 2002 ) .\n",
            "the luminosity distance in a frw metric with scale factor @xmath6 is defined as@xmath29 , \\ ] ] where the function @xmath30 $ ] is @xmath31 depending on the spatial curvature @xmath32 , respectively , and where the function @xmath33 is derived from the friedmann equation written as@xmath34 for instance , in the case of a model with matter ( subscript @xmath7 ) , dark energy ( subscript @xmath8 ) with constant equation of state @xmath35 and curvature , one has@xmath36 where @xmath37 in an empty hyperbolic universe we have then @xmath38 and@xmath39 so that the luminosity distance is@xmath40 = \\frac{z^{2}+2z}{2h_{0}}.\\ ] ] it appears then that @xmath41 for large redshifts .\n",
            "it has been shown in amendola & tocchini - valentini ( 2001 ) that , assuming @xmath35 and @xmath55 constant , the only scalar field model that reduces to the equations above requires a coupling @xmath88 with @xmath89 where the second equality holds for pressureless dark matter , @xmath71 , which is the case we study below .\n",
            "however , if the dark energy couples to baryons with strength @xmath132 then the interaction shows up to the post - post newtonian ( ppn ) order as a non - zero parameter @xmath133 defined as in hagiwara et al .  the relation between @xmath133 and @xmath132 can be found by observing that the coupled system of dark energy and matter fields @xmath134 can be derived from the lagrangian@xmath135 where the metric @xmath136 is conformally related to @xmath137 by the factor @xmath138 and where the dimensionless field @xmath139 has been introduced to match the definition of damour & esposito - farese ( 1992 ) , hagiwara et al .  ( 2002 ) and will ( 2002 ) .\n",
            "it is therefore necessary to modify the simplest case with , for instance , a modulation of the coupling parameter @xmath127 or the potential @xmath152 in order to prevent the baryon domination , as in amendola & tocchini - valentini ( 2001 ) and in amendola et al .  . these models also account for the observed level of present fluctuations .\n",
            "459\n",
            "459\n",
            "4402\n",
            "118\n",
            "abstract\n",
            "the structure of small mixed helium clusters doped with one calcium atom has been determined within the diffusion monte carlo framework . \n",
            " the results show that the calcium atom sits at the @xmath0he-@xmath1he interface . \n",
            " this is in agreement with previous studies , both experimental and theoretical , performed for large clusters . \n",
            " a comparison between the results obtained for the largest cluster we have considered for each isotope shows a clear tendency of the ca atom to reside in a deep dimple at the surface of the cluster for @xmath0he clusters , and to become fully solvated for @xmath1he clusters . \n",
            " we have calculated the absorption spectrum of ca around the @xmath2 transition and have found that it is blue - shifted from that of the free - atom transition by an amount that depends on the size and composition of the cluster .\n",
            "145\n",
            "3390\n",
            "Lex Rank Summary\n",
            "in this paper  we address the study of small mixed @xmath0he-@xmath1he clusters doped with one ca atom .\n",
            "[ solvat34 ] are plotted the ca solvation energies per helium atom as a function of the total number of helium atoms in the cluster .\n",
            "nevertheless , due to the different zero - point energy of ca and he atoms , we have found that the presence of one single ca atom causes that clusters made of any number of atoms are bound , irrespective of their bosonic or fermionic character .\n",
            "the particular case of ca atoms we are interested in has been addressed within df in pure and mixed helium clusters  @xcite .\n",
            "finally , we have used the dmc walkers to semiclassically obtain the absorption spectrum of ca around the @xmath2 transition , and have found that it is slightly blue - shifted from that of free - atom transition , with a clear dependence on the size and composition of the mixed cluster in spite of the small number of helium atoms in the studied systems .\n",
            "176\n",
            "176\n",
            "3390\n",
            "145\n",
            "abstract\n",
            "we investigate newtonian description of accreting compact bodies with hard surfaces , including luminosity and selfgravitation of polytropic perfect fluids . \n",
            " this nonlinear integro - differential problem reduces , under appropriate boundary conditions , to an algebraic relation between luminosity and the gas abundance in stationary spherically symmetric flows . \n",
            " there exist , for a given luminosity , asymptotic mass and the asymptotic temperature , two sub - critical solutions that bifurcate from a critical point . \n",
            " they differ by the fluid content and the mass of the compact centre .\n",
            "91\n",
            "3868\n",
            "Lex Rank Summary\n",
            "in a recent general - relativistic analysis  ( valid also in the newtonian limit ) the mass accretion rate @xmath0 behaves like @xmath1 , where @xmath2 is the ratio of ( roughly ) the mass of the compact core to the total mass @xcite .\n",
            "we define the eddington luminosity as that at the outermost layer of the accreting gas , that is as @xmath41 , while the total luminosity @xmath37 is equal to the product of the mass accretion rate and the total available energy per unit mass @xmath42 , where @xmath43 is an areal radius of the boundary of the compact body , @xmath44 ( @xcite ) .\n",
            "inserting that into the euler equation ( [ 1 ] )  , one finds @xmath58 thus at the sonic point the three characteristics , @xmath54 , @xmath59 and @xmath60 are related , @xmath61 it is clear from ( [ 7 ] ) that in order to have a critical flow one should have @xmath62 it is useful to express the velocity @xmath10 and the mass density @xmath20 in the following way @xmath63 where @xmath59 is the negative square root , and @xmath64 where the constant @xmath65 is equal to the mass density of collapsing fluid at the boundary @xmath66 .\n",
            "the rate of the mass accretion @xmath0 as given by ( [ dot ] ) can be expressed in terms of the characteristics of the sonic point .\n",
            "one obtains , using equations ( [ 7 ] ) and ( [ dot ] ) , that    @xmath78    now , one can can show in a way similar to that applied in the case of relativistic accretion ( @xcite ) that under the previously assumed conditions and @xmath79 one has @xmath80 for @xmath81 with some small @xmath82 .\n",
            "293\n",
            "293\n",
            "3868\n",
            "91\n",
            "abstract\n",
            "using worm - type quantum monte carlo simulations , we investigate bosonic mixtures on the triangular lattice of two species of bosons , which interact via nearest - neighbour intraspecies ( @xmath0 ) and onsite interspecies ( @xmath1 ) repulsions . for the case of symmetric hopping amplitude ( @xmath2 ) and @xmath3 \n",
            " , we determine a rich ground - state phase diagram that contains double solid , double superfluid ( 2sf ) , supersolid ( ss ) , solid - superfluid ( solid - sf ) and counterflow supersolid ( css ) states . \n",
            " the ss , solid - sf and css states exhibit spontaneous symmetry breaking among the three sublattices of the triangular lattice and between the two species , which leads to nonzero crystalline density wave order in each species . \n",
            " we furthermore show that the css and the ss states are present for @xmath4 , and the latter even survives up to @xmath5 or @xmath6 limit . \n",
            " the effects induced by the variation of @xmath7 and by the imbalance of particle numbers of the two species are also explored .\n",
            "184\n",
            "5354\n",
            "Lex Rank Summary\n",
            "the simulation is on a @xmath123 lattice , but for illustrating purpose , we show a block of @xmath124 sites.,title=\"fig:\",height=113 ]    in the region @xmath125 , the system is in the ss state and characterized by nonzero crystalline order and nonzero superfluid density for both species , as demonstrated in figs .\n",
            "in the solid - sf phase with @xmath185 , the @xmath17 species is in the solid state with filling factor @xmath186 , while the @xmath16 bosons are in the superfluid phase .\n",
            "phys .\n",
            "phys .\n",
            "phys .\n",
            "86\n",
            "86\n",
            "5354\n",
            "184\n",
            "abstract\n",
            "we analyze the mixed frame equations of radiation hydrodynamics under the approximations of flux - limited diffusion and a thermal radiation field , and derive the minimal set of evolution equations that includes all terms that are of leading order in any regime of non - relativistic radiation hydrodynamics . \n",
            " our equations are accurate to first order in @xmath0 in the static diffusion regime . \n",
            " in contrast , we show that previous lower order derivations of these equations omit leading terms in at least some regimes . in comparison to comoving frame formulations of radiation hydrodynamics , \n",
            " our equations have the advantage that they manifestly conserve total energy , making them very well - suited to numerical simulations , particularly with adaptive meshes . for systems in the static diffusion regime \n",
            " , our analysis also suggests an algorithm that is both simpler and faster than earlier comoving frame methods . \n",
            " we implement this algorithm in the orion adaptive mesh refinement code , and show that it performs well in a range of test problems .\n",
            "175\n",
            "15201\n",
            "Lex Rank Summary\n",
            "this may not be the case for an optically thin system , or one in which line transport is important , but since we are limiting our application to systems to which we can reasonably apply the diffusion approximation , this is not a major limitation .\n",
            "in the comoving frame in an optically thick system ,  one is in the static diffusion regime , so @xmath149 .\n",
            "they are accurate to first order in @xmath34 in the static diffusion limit , since we have had to retain all order @xmath34 terms in this limit because they are of leading order in dynamic diffusion problems .\n",
            "to compare this to our mixed frame radiation energy equation ( [ radenergy ] )  , we replace the comoving frame energy @xmath64 in ( [ firstlaw ] ) with the lab frame energy @xmath45 using the lorentz transformation ( [ etransform ] ) and retain all terms that are of leading order in any regime .\n",
            "as an initial check of the gas - radiation energy exchange in our code in a case  when radiation pressure is not significant and the gas is at rest , we simulate the non - equilibrium marshak wave problem .\n",
            "199\n",
            "199\n",
            "15201\n",
            "175\n",
            "abstract\n",
            "we present 40 quasar absorption line systems at intermediate redshifts ( @xmath0 ) , with focus on one of the most kinematically complex known , as examples of how the unique capabilities of space  based and ground  based facilities can be combined to glean much broader insights into astrophysical systems .\n",
            "51\n",
            "919\n",
            "Lex Rank Summary\n",
            "the ism and halos of local galaxies are comprised of many ionization phases , including diffused ionized gas , extended coronae , and denser low ionization regions often located in front of shock fronts ( e.g.dahlem 1998 ) .\n",
            ", are redshifted to the near uv ; a study of the high ionization component requires a spaced  based telescope , i.e.  _ hst_.\n",
            "the three systems at @xmath15 , @xmath16 , and @xmath17 along the line of sight to pg  @xmath18 exhibit complex kinematics and exceptionally strong , , and absorption .\n",
            "in the top panels of figure  2 ,  the hires / keck spectra of the @xmath19 transition and of the mg0.1emii  @xmath20 doublet are shown with a voigt profile model spectrum superimposed ; the ticks give the component centers .\n",
            "the solid spectrum is a two  phase model , which allows the higher ionization gas to reside in a separate phase .\n",
            "150\n",
            "150\n",
            "919\n",
            "51\n",
            "abstract\n",
            "we solve one of the open problems in einstein - cartan theory , namely we find a natural matter source whose spin angular momentum tensor is compatible with the cosmological principle . \n",
            " we analyze the resulting evolution equations and find that an epoch of accelerated expansion is an attractor . \n",
            " the torsion field quickly decays in that period . \n",
            " our results are interpreted in the context of the standard model of cosmology .\n",
            "73\n",
            "2771\n",
            "Lex Rank Summary\n",
            "the torsion tensor is defined as the skew - symmetric part of the ( full ) connection @xmath23 } =        \\frac{1}{2 } \\bigl(\\tilde{\\gamma}^\\lambda_{\\mu\\nu}-        \\tilde{\\gamma}^\\lambda_{\\nu\\mu } \\bigr ) ,        \\label{eq : t1b}\\end{aligned}\\ ] ] and in turn we can decompose the connection into the christoffel symbol and an additional piece , the contortion tensor @xmath24 combining the latter relation with the definition of torsion  ( [ eq : t1b ] ) , it follows that torsion and contortion are algebraically related by @xmath25    the covariant derivative when acting on a spinor is defined by @xmath26 where @xmath27 and @xmath28 $ ] are the generators of the lorentz group .\n",
            "the anholonomic and holonomic connections are related by @xmath29 we use the @xmath30-matrices in the chiral form @xmath31 with @xmath32 , and the @xmath30-matrices satisfy @xmath33    the action of einstein - cartan gravity is @xmath34 where @xmath35 is the ricci scalar computed from the complete connection with contortion contributions , @xmath36 is the determinant of the metric , @xmath37 denotes the matter lagrangian and @xmath38 is the coupling constant ; the speed of light is set to one @xmath39 .\n",
            "the resulting field equations are @xmath40 where @xmath41 is the spin angular momentum tensor , defined by @xmath42 and @xmath43 is the total energy - momentum tensor @xmath44 where @xmath45 is metric energy - momentum tensor @xmath46 the field equations  ( [ eq : t9 ] ) are in general 24 algebraic equations , and in the absence of spin sources torsion vanishes , torsion does not propagate .\n",
            "this then implies the following non - vanishing anholonomic christoffel symbols @xmath54 to be @xmath55 when the cosmological principle is applied to the torsion tensor  @xcite the allowed components reduce to @xmath56 the cosmological einstein tensor with torsion is now given by @xmath57    in addition to the geometry , also the matter has to be compatible with homogeneity and isotropy .\n",
            "the torsion functions @xmath64 and @xmath65 can therefore be expressed   in terms of the matter @xmath66 which can be combined to give @xmath67 therefore , a dark ghost spinor field satisfying the cosmological principle indeed yields non - trivial contributions to the spatial axial torsion component and to the time component of the torsion vector .\n",
            "370\n",
            "370\n",
            "2771\n",
            "73\n",
            "abstract\n",
            "quantum spin hall insulator / metal interfaces are naturally formed in graphene ribbons with intrinsic spin - orbit coupling by selectively doping two regions creating a potential step . for a clean graphene ribbon , the transmission of the topological edge states through a n - n or p - p junction is perfect irrespective of the ribbon termination , width , and potential step parameters due to the orthogonality of incoming and outgoing edge channels . \n",
            " this is shown numerically for an arbitrary crystallographic orientation of the ribbon and proven analytically for zigzag and metallic armchair boundary conditions . \n",
            " in disordered ribbons , the orthogonality between left- and right - movers is in general destroyed and backscattering sets in . \n",
            " however , perfect transmission is restored by increasing the ribbon s width , even in the presence of strong edge roughness .\n",
            "143\n",
            "9399\n",
            "Lex Rank Summary\n",
            "b ) energy bands for a zigzag terminated ribbon at the left and right sides of a potential step of height @xmath0 and width @xmath2 .\n",
            "in our case of a constant spin - orbit coupling and a potential step  we can only state that numerically we also observe perfect transmission as long as the ribbon is metallic in the presence of spin - orbit coupling , i.e. , @xmath83 , even though the isospins of the incoming and outgoing edge states are not orthogonal .\n",
            "we find that the wavefunction at the lower boundary @xmath84 can be written as @xmath88.\\ ] ] it is interesting to note that one needs a superposition of two plane waves in order to satisfy the boundary conditions , both for the armchair and the zigzag ribbon .\n",
            "we have found that for clean ballistic ribbons ( with arbitrary crystallographic orientation ) , the topological edge states are transmitted perfectly through such a junction , independent of the ribbon s width , the parameters of the potential step and the value of the intrinsic spin - orbit coupling , as long as inter - valley scattering is not present .\n",
            "moreover , we prove the orthogonality between same spin left and right moving edge states at the opposite boundaries of the ribbon and obtain the edge state width as a function of spin - orbit coupling and energy .\n",
            "231\n",
            "231\n",
            "9399\n",
            "143\n",
            "abstract\n",
            "we calculate the in - medium masses of the bottomonium states ( @xmath0 , @xmath1 , @xmath2 and @xmath3 ) in isospin asymmetric strange hadronic matter at finite temperatures . \n",
            " the medium modifications of the masses arise due to the interaction of these heavy quarkonium states with the gluon condensates of qcd . \n",
            " the gluon condensates in the hot hadronic matter are computed from the medium modification of a scalar dilaton field within a chiral su(3 ) model , introduced in the hadronic model to incorporate the broken scale invariance of qcd . \n",
            " there is seen to be drop in the masses of the bottomonium states and mass shifts are observed to be quite considerable at high densities for the excited states . \n",
            " the effects of density , isospin asymmetry , strangeness as well as temperature of the medium on the masses of the @xmath4-states are investigated . \n",
            " the effects of the isospin asymmetry as well as strangeness fraction of the medium are seen to be appreciable at high densities and small temperatures . \n",
            " the density effects are the most dominant medium effects which should have observable consequences in the compressed baryonic matter ( cbm ) in the heavy ion collision experiments in the future facility at fair , gsi . \n",
            " the study of the @xmath4 states will however require access to energies higher than the energy regime planned at cbm experiment . \n",
            " the density effects on the bottomonium masses should also show up in the dilepton spectra at the sps energies , especially for the excited states for which the mass drop is observed to quite appreciable . \n",
            " # 1\n",
            "271\n",
            "7186\n",
            "Lex Rank Summary\n",
            "in the non - relativistic limit , due to vanishing of the contribution from the magnetic field  , the expectation value of the scalar gluon condensate can be expressed in terms of the color electric field and hence the mass shift formula for the bottomonium states can be written in terms of the difference in the value of the scalar gluon condensate in the medium and in the vacuum as @xcite @xmath75    in the present investigation , the wave functions for the bottomonium states are taken to be gaussian and are given as @xcite @xmath76 where @xmath77 is the parameter describing the strength of the harmonic oscillator potential , @xmath78 is the reduced mass of the bottom quark and bottom anti - quark system , @xmath79 is the associated laguerre polynomial .\n",
            "this is shown for different values of the temperature for typical values of the strangeness fraction of the medium , @xmath87 , in subplots ( a ) , ( c ) and ( e ) for the isospin symmetric matter and in subplots ( b ) , ( d ) and ( f ) for the isospin asymmetric matter with @xmath88=0.5 .\n",
            "in figure  [ ggscdens ] , the density dependence of the scalar gluon condensate , @xmath95 is shown for temperatures , t=0 , 100 and 150 mev , for the isospin symmetric matter in subplots ( a ) , ( c ) and ( e ) , for values of the strangeness fraction , @xmath87 as 0 , 0.3 and 0.5 .  these are compared with the values for the isospin asymmetric matter with @xmath88=0.5 plotted in ( b ) , ( d ) and ( f ) .\n",
            "phys .\n",
            "phys , j. a * 41 * , 205 ( 2009 ) .\n",
            "294\n",
            "294\n",
            "7186\n",
            "271\n",
            "abstract\n",
            "we investigate the no - boundary measure in the context of moduli stabilization . to this end , we first show that for exponential potentials , there are no classical histories once the slope exceeds a critical value . \n",
            " we also investigate the probability distributions given by the no - boundary wave function near maxima of the potential . \n",
            " these results are then applied to a simple model that compactifies @xmath0d to @xmath1d ( hbsv model ) with fluxes . \n",
            " we find that the no - boundary wave function effectively stabilizes the moduli of the model .    moreover , we find the _ a priori _ probability for the cosmological constant in this model . \n",
            " we find that a negative value is preferred , and a vanishing cosmological constant is not distinguished by the probability measure . \n",
            " we also discuss the application to the cosmic landscape . \n",
            " our preliminary arguments indicate that the probability of obtaining anti de sitter space is vastly greater than for de sitter .\n",
            "168\n",
            "8865\n",
            "Lex Rank Summary\n",
            "then we have @xmath16 the hbsv model has two essential properties in this context : ( 1 ) it has one moduli field that is stabilized by a potential and ( 2 ) as one increases the number of fluxes , one can change the vacua from anti de sitter to de sitter .\n",
            "now we will investigate some properties of the probability distribution on histories given by the no - boundary wave function for einstein gravity coupled to a scalar field .\n",
            "for a typical form of the moduli potential @xmath151 where @xmath152s are polynomials of @xmath26 and @xmath153s are constants  , we require the condition @xmath154  if this condition does not hold , then the no - boundary measure can not explain the stabilization of moduli fields .\n",
            "[ [ anti - de - sitter - catastrophe - and - the - no - boundary - measure ] ] anti de sitter catastrophe and the no - boundary measure + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + + +    if there is a local maximum with a very small vacuum energy of a potential that is allowed from string theory , then around the point will give @xmath210 parameter .\n",
            "these two observations are applied to the hbsv model : classical histories are allowed only for the local maximum , and the probability will not crucially depend on the initial conditions ( fast - rolling fuzzy instantons ) .\n",
            "281\n",
            "281\n",
            "8865\n",
            "168\n",
            "abstract\n",
            "we argue that the properties of the type ia supernova ( sn ia ) sn  2011fe can be best explained within the frame of the core - degenerate ( cd ) scenario . in the cd scenario a white dwarf ( wd ) merges with the core of an asymptotic giant branch ( agb ) star and forms a rapidly rotating wd , with a mass close to and above the critical mass for explosion . \n",
            " rapid rotation prevents immediate collapse and/or explosion . spinning down over a time of @xmath0 \n",
            " yr brings the wd to explosion . \n",
            " a very long delayed explosion to post - crystallization phase , which lasts for about @xmath1 , leads to the formation of a highly carbon - enriched outer layer . \n",
            " this can account for the carbon - rich composition of the fastest - moving ejecta of sn  2011fe . in reaching the conclusion that the cd scenario best explains the observed properties of sn  2011fe we consider both its specific properties , like a very compact exploding object and carbon rich composition of the fastest - moving ejecta , and the general properties of sne ia . \n",
            " supernovae : general  supernovae : individual ( sn  2011fe )\n",
            "205\n",
            "3317\n",
            "Lex Rank Summary\n",
            "in section  [ sec : carbon ] we discuss how the fastest ejecta of sn  2011fe can be enriched in carbon , as a consequence of carbon - oxygen phase separation upon crystallization .\n",
            "however , this does not solve other problems of the sd scenario , such as that it is expected to explain only a small fraction of sne ia , and that it is not clear that the wd can grow by accretion to the chandrasekhar mass limit .\n",
            "the carbon - rich fastest ejecta is also problematic for models based on helium accretion , such as the ddet scenario @xcite .\n",
            "by that time the luminosity of the wd is @xmath21 ,  its effective temperature is @xmath22 , and it has an outer layer of mass @xmath23 where the carbon mass abundance is @xmath24 ( fig .\n",
            "@xcite  considered a merge of a wd with a core of an agb star to explain the formation of massive rotating wds with strong magnetic fields , and @xcite commented that such wds might be more likely to form sn ia .\n",
            "179\n",
            "179\n",
            "3317\n",
            "205\n",
            "abstract\n",
            "we present an apparatus that converts every pulse of a pulsed light source to a pulse train in which the intensities of the different pulses are samples of the spatial or temporal frequency spectrum of the original pulse . in this way \n",
            " , the spectrum of the incident light can be measured by following the temporal response of a single detector . \n",
            " the apparatus is based on multiple round - trips inside a 2f - cavity - like mirror arrangement in which the spectrum is spread on the back focal plane , where after each round - trip a small section of the spectrum is allowed to escape . \n",
            " the apparatus is fibre - free , offers easy wavelength range tunability , and a prototype built achieves over 10% average efficiency in the near infra red . \n",
            " we demonstrate the application of the prototype for the efficient measurement of the joint spectrum of a non - degenerate bi - photon source in which one of the photons is in the near infra red .\n",
            "174\n",
            "3630\n",
            "Lex Rank Summary\n",
            "[ fig1](a ) .\n",
            "[ fig1](c ) , due to the horizontal tilt of mirror m3 , every time the light hits mirror m4 , its horizontal position is shifted by @xmath0 , where @xmath1 is the tilt angle of m3 , and @xmath2 is the focal length of the lens .\n",
            "in this way  , a single , multicolour pulse at the input is divided into a train of pulses at the output , each of a different colour range , separated by one round trip time.,scaledwidth=47.0% ]  for building a scissors prototype we have used the following optical arrangements .\n",
            "the sharpness of the input and output mirror edges was found to be about 50  @xmath8 m . in order to reduce relative scattering losses on the edge of mirror m4 to about 10% , the tilt angle of mirror m3  was chosen such that the round - trip horizontal shift on mirror m4 was about 500  @xmath8 m .  this set the spectral bin size to about 1 nm .\n",
            "[  fig2](a ) by comparing the total count rate measured at the scissors output to that measured at its input , and was found to be @xmath1510@xmath16 .\n",
            "197\n",
            "197\n",
            "3630\n",
            "174\n",
            "abstract\n",
            "we consider fermion - dimer scattering in the presence of a large positive scattering length in the frame of functional renormalization group equations . \n",
            " a flow equation for the momentum dependent fermion - dimer scattering amplitude is derived from first principles in a systematic vertex expansion of the exact flow equation for the effective action . \n",
            " the resummation obtained from the nonperturbative flow is shown to be equivalent to the one performed by the integral equation by skorniakov and ter - martirosian ( stm ) . \n",
            " the flow equation approach allows to integrate out fermions and bosons simultaneously , in line with the fact that the bosons are not fundamental but build up gradually as fluctuation induced bound states of fermions . \n",
            " in particular , the stm result for atom - dimer scattering is obtained by choosing the relative cutoff scales of fermions and bosons such that the fermion fluctuations are integrated out already at the initial stage of the rg evolution .\n",
            "163\n",
            "8383\n",
            "Lex Rank Summary\n",
            "in order to see this  , we consider the momentum independent parts in both the fermion and the boson propagator , @xmath68 ( the `` chemical potential '' for the fermions in vacuum ) and @xmath69 , which act as gaps for the propagation of fermions and bosons .\n",
            "on the other hand  , we find that the flow in the four - particle sector , described by the dimer - dimer vertex , is affected by the fermion - dimer vertex .\n",
            "( [ atomdimersimplified ] ) thus reduces to @xmath153 , which can be brought in a closed form for @xmath154 since @xmath155 is @xmath156-independent in the above limit , @xmath157 this equation can be integrated straightforwardly with the result @xmath158 here @xmath109 denotes the full fermion - dimer vertex in the limit @xmath159 where all fluctuations are included .\n",
            "a further goal is the treatment of the four - body problem in the presence of a positive scattering length , i.e. , dimer - dimer scattering @xcite .\n",
            "a * 367 * 263 - 267 ( 2007 ) .\n",
            "178\n",
            "178\n",
            "8383\n",
            "163\n",
            "abstract\n",
            "like a three - qubit greenberger - horne - zeilinger(ghz ) symmetry we explore a corresponding symmetry in the four - qubit system , which we call ghz@xmath0 symmetry . while whole ghz - symmetric states can be represented by two real parameters , the whole set of the ghz@xmath0-symmetric states \n",
            " is represented by three real parameters . in the parameter space \n",
            " all ghz@xmath0-symmetric states reside inside a tetrahedron . \n",
            " we also explore a question where the given slocc class of the ghz@xmath0-symmetric states resides in the tetrahedron . among nine slocc classes we have examined five slocc classes , which results in three linear hierarchies @xmath1 , @xmath2 , and @xmath3 which hold , at least , in the whole set of the ghz@xmath0-symmetric states . \n",
            " difficulties arising in the analysis of the remaining slocc classes are briefly discussed .\n",
            "141\n",
            "7269\n",
            "Lex Rank Summary\n",
            "in appendix  a we use this state to show that when @xmath18 and @xmath16 are given , the @xmath25 class of the ghz@xmath0-symmetric states resides in @xmath63 , where @xmath64 in eq .\n",
            "in appendix  b we use this state to show that when @xmath18 and @xmath16 are given , the @xmath26 class of the ghz@xmath0-symmetric states resides in @xmath63 , where @xmath75 .\n",
            "in appendix c  we use this state to show that when @xmath18 and @xmath16 are given , the @xmath27 class of the ghz - symmetric states resides in @xmath63 , where @xmath80 .\n",
            "in appendix d we use this state to show that when @xmath18 and @xmath16 are given , the @xmath28 class of the ghz@xmath0-symmetric states resides in @xmath63 , where @xmath95 however , the region generated by eq .\n",
            "in appendix  e we use this state to show that when @xmath18 and @xmath16 are given , the @xmath29 class of the ghz@xmath0-symmetric states resides in @xmath63 .\n",
            "159\n",
            "159\n",
            "7269\n",
            "141\n",
            "abstract\n",
            "we report how strategic evolution can stabilize topological states in a network of fitzhugh - nagumo systems . \n",
            " the evolution follows a repeated process of adding or deleting of links between two nodes that is decided based on a threshold set for the closeness between them . \n",
            " this results in a need based rewiring that keeps the systems in synchrony in a single cluster or in phase locked states in different clusters . \n",
            " we analyse in detail the occurrence of such multi stable topological fixed points with corresponding emergent dynamical states using the frequency of occurrence of each state when evolved from a large number of initial states . \n",
            " we find that there is an optimum range for the threshold used in the strategy that results in maximum frequency for the stable topological states .\n",
            "135\n",
            "6223\n",
            "Lex Rank Summary\n",
            "we introduce a strategy for evolving the system in which in addition to the dynamical evolution of the nodes , a new network topology is selected after a rewiring time of @xmath13 .\n",
            "the time series from all the nodes for this state is shown in fig .\n",
            "we mention that the fixed point nature is in the topology and not in the nodal dynamics since even in the final state , the nodes in the topological fixed point will have dynamics as given by eq .\n",
            "this means that , by properly choosing the parameters @xmath65 and @xmath13 , the systems can be driven from one topology of anti phase state to the other of in phase state .\n",
            "similarly , we illustrate this for the @xmath20 cluster state for the specific case of @xmath31 , @xmath31 cluster in fig .\n",
            "138\n",
            "138\n",
            "6223\n",
            "135\n",
            "abstract\n",
            "we show that elliptic second order operators @xmath0 of divergence type fulfill maximal parabolic regularity on distribution spaces , even if the underlying domain is highly non - smooth , the coefficients of @xmath0 are discontinuous and @xmath0 is complemented with mixed boundary conditions . applications to quasilinear parabolic equations with non - smooth data are presented .\n",
            "58\n",
            "18122\n",
            "Lex Rank Summary\n",
            "thus , @xmath239 also has a bounded @xmath219-calculus on @xmath1 with @xmath219-angle @xmath5 for all @xmath240 by @xcite .\n",
            "4 .  if @xmath473 is a generator of an analytic semigroup on a banach space @xmath70 , we define @xmath474 by @xmath475 then , by definition of the distributional time derivative , it is easy to see that @xmath69 has maximal parabolic regularity on @xmath70 if and only if the operator @xmath476 continuously extends to an operator from @xmath467 into itself .\n",
            "as the right hand side of  is in fact from @xmath649 , this implies that there is a unique function @xmath650 which satisfies @xmath651 and @xmath652 as an equation in @xmath649 .\n",
            "then @xmath0 also satisfies maximal parabolic regularity on any of the interpolation spaces @xmath764_\\theta , \\quad   \\theta \\in [ 0,1],\\ ] ] or @xmath765 , \\          s \\in \\left ] 1 , \\infty \\right[.\\ ] ]    1 .   by lemma  [ l - relativ ] ,  if @xmath766 , then @xmath767 is well defined and one has the equality @xmath768 by definition of @xmath0 .\n",
            "if one defines the coefficient function @xmath34 as @xmath1039 on the first beam , and as @xmath1040 on the other , then , due to proposition  [ p - geo3d ]  iii ) , @xmath1041 provides a topological isomorphism for some @xmath984 , if one can show that @xmath1042 is a lipschitz domain .\n",
            "228\n",
            "228\n",
            "18122\n",
            "58\n",
            "abstract\n",
            "we present a theoretical study of the energy levels in a parabolically confined quantum dot in the presence of the rashba spin - orbit interaction ( soi ) . \n",
            " the features of some low - lying states in various strengths of the soi are examined at finite magnetic fields . \n",
            " the presence of a magnetic field enhances the possibility of the spin polarization and the soi leads to different energy dependence on magnetic fields applied . \n",
            " furthermore , in high magnetic fields , the spectra of low - lying states show basic features of fock - darwin levels as well as landau levels .\n",
            "104\n",
            "3698\n",
            "Lex Rank Summary\n",
            "it has been realized that in contrast to the diluted magnetic semiconductors in which the soi is induced by the presence of an external magnetic field , spin splitting of carriers can be achieved in narrow - gap semiconductor nanostructures even in the absence of the magnetic field .\n",
            "in the present study , we examine the dependence of the energy levels and the occupation of electrons to different states on the strength of the soi and of the magnetic field in a few - electron quantum dot system .\n",
            "the presence of the magnetic field reduces the spin polarization and a fully spin - polarized ten - electron dot is achieved at @xmath63 ev@xmath56m.,scaledwidth=45.0% ]    when a perpendicular d.c .  magnetic field is applied to a quantum dot , the nature of spin - dependent energy spectrum can become even richer in terms of physics due to the coupling of the magnetic field to the confining potential of the quantum dot and to the potential induced by soi .\n",
            "thus , ( 1 ) the strong spin polarization can be achieved in a weakly confined dot at zero and non - zero magnetic fields ; ( 2 ) the characteristics of the fock - darwin scheme and the landau type levels are revealed when the magnetic field is strong enough ; and ( 3 ) the effective soi in the system decreases with increasing magnetic field and confining potential of the dot .\n",
            "on the basis that the energy levels in spin - degenerate quantum dot systems have been well studied using optical and optoelectronic measurements , we believe these experimental techniques can also be used to examine the energy spectra of a quantum dot with soi .\n",
            "285\n",
            "285\n",
            "3698\n",
            "104\n",
            "abstract\n",
            "using the sample from the _ redshift one ldss3 emission line survey ( roles ) , we probe the dependence of star formation rate ( sfr ) and specific star formation rate ( ssfr ) as a function of stellar mass @xmath0 and environment as defined by local galaxy density , in the cdfs field . \n",
            " our spectroscopic sample consists of 312 galaxies with @xmath1 , corresponding to stellar mass @xmath2 , and with [ oii ] derived star - formation rates sfr@xmath3yr , at @xmath4 . \n",
            " the results have been compared directly with the sloan digital sky survey stripe 82 sample at @xmath5 . for star - forming galaxies , \n",
            " we confirm that there is little correlation between sfr and density at @xmath6 . \n",
            " however , for the lowest mass galaxies in our @xmath7 sample , those with @xmath8 , we find that both the median sfr and specific sfr _ increase _ \n",
            " significantly with increasing local density . \n",
            " the `` downsizing '' trend for low mass galaxies to be quenched progressively later in time appears to be more pronounced in moderately overdense environments . \n",
            " overall we find that the evolution of star - formation in galaxies is most strongly driven by their stellar mass , with local galaxy density playing a role that becomes increasingly important for lower mass galaxies . \n",
            " _    galaxies : evolution , stellar content\n",
            "230\n",
            "10945\n",
            "Lex Rank Summary\n",
            "in papers i and ii , we have constructed a sample of star forming galaxies with stellar mass between @xmath22 and @xmath23 at @xmath7 using the [ oii]@xmath243727 emission line luminosity to derive the sfr .\n",
            "for the few galaxies in our roles catalogue that do not have fireworks redshifts , we use the photo - z from which our survey was initially selected , @xcite , as described in paper  ii .\n",
            "thus , in figure  [ fig : ssfr_combined ] , we show ssfr as a function of stellar mass and @xmath73 ; both roles and sdss show that the ssfr decreases with @xmath0 .\n",
            "we show the average sfr and ssfr as a function of @xmath68 with @xmath75=5 in the stacked regions in fig .\n",
            "we thus consider the sfr and ssfr of our lowest  mass galaxies in the @xmath12 sample , @xmath132log(@xmath15)@xmath133 .\n",
            "143\n",
            "143\n",
            "10945\n",
            "230\n",
            "abstract\n",
            "motivated by recent interest in their applications , we report a systematic study of cs atomic properties calculated by a high - precision relativistic all - order method . \n",
            " excitation energies , reduced matrix elements , transition rates , and lifetimes are determined for levels with principal quantum numbers @xmath0 and orbital angular momentum quantum numbers @xmath1 . recommended values and estimates of uncertainties \n",
            " are provided for a number of electric - dipole transitions and the electric dipole polarizabilities of the @xmath2 , @xmath3 , and @xmath4 states . \n",
            " we also report a calculation of the electric quadrupole polarizability of the ground state . \n",
            " we display the dynamic polarizabilities of the @xmath5 and @xmath6 states for optical wavelengths between 1160  nm and 1800  nm and identify corresponding magic wavelengths for the @xmath7 , @xmath8 transitions . \n",
            " the values of relevant matrix elements needed for polarizability calculations at other wavelengths are provided .\n",
            "152\n",
            "3566\n",
            "Lex Rank Summary\n",
            "we calculated lifetimes of the @xmath27 , @xmath28 , @xmath29 , and @xmath30 states in cs using out final values of the matrix elements listed in table  [ table1 ] and experimental energies from  @xcite .\n",
            "the valence contribution to frequency - dependent scalar @xmath106 and tensor @xmath107 polarizabilities  is evaluated as the sum over intermediate @xmath88 states allowed by the electric - dipole selection rules  @xcite @xmath108 where @xmath109 is given by @xmath110 in the equations above , @xmath111 is assumed to be at least several linewidths off resonance with the corresponding transitions and @xmath112 are the reduced electric - dipole matrix elements .\n",
            "contributions to the polarizabilities of the @xmath23 , @xmath25 levels , @xmath114 and @xmath115 state of cesium are given in the supplemental material @xcite .\n",
            "in this work  , we present several other magic wavelengths for for the @xmath7 and @xmath8 transitions in cs .\n",
            "to determine the uncertainty in the values of magic wavelengths , we first determine the uncertainties in the polarizability values at the magic wavelengths  then , the uncertainties in the values of magic wavelengths are determined as the maximum differences between the central value and the crossings of the @xmath166 and @xmath167 curves , where the @xmath168 are the uncertainties in the corresponding @xmath5 and @xmath6 polarizabilities .\n",
            "214\n",
            "214\n",
            "3566\n",
            "152\n",
            "abstract\n",
            "in this paper we analyze the stellar populations present in m31 using nine sets of adjacent hst - nicmos camera 1 and 2 fields with galactocentric distances ranging from @xmath0 to @xmath1 . \n",
            " these infrared observations provide some of the highest spatial resolution measurements of m31 to date ; our data place tight constraints on the maximum luminosities of stars in the bulge of m31 . \n",
            " the tip of the red giant branch is clearly visible at @xmath2 , and the tip of the asymptotic giant branch ( agb ) extends to @xmath3 . \n",
            " this agb peak luminosity is significantly fainter than previously claimed ; through direct comparisons and simulations we show that previous measurements were affected by image blending . \n",
            " we do observe field - to - field variations in the luminosity functions , but simulations show that these differences can be produced by blending in the higher surface brightness fields . \n",
            " we conclude that the red giant branch of the bulge of m31 is not measurably different from that of the milky way s bulge . \n",
            " we also find an unusually high number of bright blueish stars ( 7.3 arcmin@xmath4 ) which appear to be galactic foreground stars .\n",
            "201\n",
            "13014\n",
            "Lex Rank Summary\n",
            "the ratio of giants to lpvs for each of our nic2 fields is shown in figure [ fig : lpvs ] as a function of bulge / disk ratio .\n",
            "in order to better understand the relationship between the groundbased photometry and our nicmos measurements we have performed a star - by - star comparison of the objects measured by rmg93 in field 1 . as is obvious from figure  [ fig : field1matchup ] , none of the objects seen from the ground correspond to single stars in the nicmos image .\n",
            "field 3 is not as severe , however the groundbased observations predict that we should find many more bright stars up to @xmath20 mag brighter than we see .\n",
            "these simulations show that for the most crowded fields we can expect the brightening due to blending to be as high as 0.75 magnitudes in @xmath76 and 0.55 magnitudes in @xmath21 .\n",
            "in a comparison of our f174 and f177 lfs with the recently observed bulge field of @xcite , we find that the @xmath20 magnitude difference between his and our lfs is due entirely to blending in his lower resolution observations , rather than a calibration error as claimed by davidge  .\n",
            "201\n",
            "201\n",
            "13014\n",
            "201\n",
            "abstract\n",
            "we investigate a phase - reference vlbi observation that was conducted at 15.4  ghz by fast switching vlba antennas between the compact steep - spectrum radio source 3c 138 and the quasar pks 0528 + 134 which are about 4@xmath0 away on the sky . by comparing the phase - reference mapping with the conventional hybrid mapping , \n",
            " we demonstrate the feasibility of high precision astrometric measurements for sources separated by 4@xmath0 . \n",
            " vlbi phase - reference mapping preserves the relative phase information , and thus provides an accurate relative position between 3c 138 and pks 0528 + 134 of @xmath1 and @xmath2 ( j2000.0 ) in right ascension and declination , respectively . \n",
            " this gives an improved position of the nucleus ( component a ) of 3c 138 in j2000.0 to be ra=@xmath3 and dec=@xmath4 under the assumption that the position of calibrator pks 0528 + 134 is correct . \n",
            " we further made a hybrid map by performing several iterations of clean and self - calibration on the phase - referenced data with the phase - reference map as an input model for the first phase self - calibration . compared with the hybrid map from the limited visibility data directly obtained from fringe fitting 3c 138 data \n",
            " , this map has a similar dynamic range , but a higher angular resolution . \n",
            " therefore , phase - reference technique is not only a means of phase connection , but also a means of increasing phase coherence time allowing self - calibration technique to be applied to much weaker sources .\n",
            "261\n",
            "3482\n",
            "Lex Rank Summary\n",
            "from the phase - reference map , we also estimate the relative separation between the target source 3c 138 and the calibrator pks 0528 + 134 , from which an improved coordinate of 3c 138 is obtained .\n",
            "the results are listed in tables 1 and 2 along with some parameters of each map in table 3 .      as the consequence of the coherence loss due to the temporal phase fluctuation and large angular separation between the target and reference sources , the phase - referenced map ( fig.1(a ) ) reveals only two brighter components ( a and b1 ) of the four well detected vlbi components ( a , b1 , b2 , and c ) shown in the hybrid maps of 3c  138 by shen et al .  ( 2005 ) .\n",
            "the uv - coverage plots in fig.2 ( also refer to table 3 ) reveal that the resolutions of fig.1(a ) and fig.1(b ) are about 4 and 2 times higher than that of fig.2 of shen et al .  ( 2005 ) in right ascension and declination , respectively .\n",
            "it should be mentioned that although a similar offset is also seen in fig.1(b ) , it can not be used to estimate the relative position since some iterations of phase self - calibration have been invoked in the mapping process .\n",
            "this provides an improved position of 3c 138 to be @xmath3 and @xmath26 ( j2000.0 ) in right ascension and declination , respectively , under the assumption that there is no error in the position of the strong reference source pks 0528 + 134 .    by comparing the hybrid maps  made from the visibility data with and without applying phase - reference technique , we found that both maps have a similar dynamic range , but the hybrid map from the phase - referenced data has a higher angular resolution since more visibility data are recovered .\n",
            "321\n",
            "321\n",
            "3482\n",
            "261\n",
            "abstract\n",
            "we consider spin rotations in single- and two - electron quantum dots that are driven by external ac electric field with two mechanisms that couple the electron spatial motion and the spin degree of freedom : the spin - orbit interaction and a random fluctuation of the overhauser field due to nuclear spin bath . we perform a systematic numerical simulation of the driven system using a finite difference approach with an exact account taken for the electron - electron correlation . \n",
            " the simulation demonstrates that the electron oscillation in fluctuating nuclear field is translated into an effective magnetic field during the electron wave packet motion . \n",
            " the effective magnetic field drives the spin transitions according to the electric - dipole spin resonance mechanism . \n",
            " we find distinct signatures of selection rules for direct and higher - order transitions in terms of the spin - orbital symmetries of the wave functions . \n",
            " the selection rules are violated by the random fluctuation of the overhauser field .\n",
            "166\n",
            "5061\n",
            "Lex Rank Summary\n",
            "in this configuration the orbital effects of the external magnetic field can be neglected , and the single - electron hamiltonian takes the form , @xmath3 where @xmath4 is the confinement potential , @xmath5 is the potential of the ac electric field which will drive the spin transitions , @xmath6 , @xmath7 describes the interaction of the electron spin with the overhauser field @xmath8 @xmath9 and @xmath10 introduces the linear rashba spin - orbit interaction due to the electric field oriented @xmath11 perpendicular to the length of the quantum dot @xmath12 we apply gaas material parameters with the effective electron mass @xmath13 , and the lande factor @xmath14 .\n",
            "the evolution of the system in time is given by the schrdinger equation @xmath40 , which is solved with the explicit askar - cakmak scheme@xcite @xmath41      in gaas each nucleus of the crystal lattice carry an uncompensated spin that interacts with the electron spin via the fermi contact hyperfine interaction,@xcite @xmath42 , where @xmath43 is the position of k - th nucleus , @xmath44 and @xmath45 are the nuclear and electron spin operators , and @xmath46 is the coupling constant which is proportional to the magnetic moment of nucleus @xmath47 and the probability density of finding the electron therein .\n",
            "figure [ wije](a ) shows the single - electron energy spectrum for a quantum dot of length 158.2 nm as a function of the magnetic field .\n",
            "phys .\n",
            "frolov , and l. p. kouwenhoven , phys .\n",
            "243\n",
            "243\n",
            "5061\n",
            "166\n",
            "abstract\n",
            "fragmentation functions ( ffs ) describe the formation of final state particles from a partonic initial state \n",
            " . precise knowledge of these functions is a key ingredient in accessing quantities such as the nucleon spin structure in semi - inclusive deep - inelastic scattering and proton proton collisions . \n",
            " however , fragmentation functions can currently not be determined from first principles quantum chromodynamics and have to be extracted from experimental data . \n",
            " the belle experiment at kek , japan , provides a large data sample for high precision measurements on @xmath0 annihilations allowing for first - time or more precise extractions of fragmentation functions . \n",
            " analyses for extractions of spin - independent ( unpolarized ffs ) as well as spin - dependent fragmentation functions ( interference ffs ) at belle are presented .\n",
            "133\n",
            "1433\n",
            "Lex Rank Summary\n",
            "the likelihood cut selections yield fairly accurate pid but need to be calibrated in the context of a high precision measurement , such that measured hadron yields can be corrected for particle misidentification .\n",
            "complete @xmath11 matrices of pid probabilities are extracted from experimental data for species @xmath15 by analyzing decays of @xmath16 , @xmath17 and @xmath18 particles .\n",
            "the pid probability matrices from all kinematic areas are inverted and then applied to the measured yields @xmath25 to obtain pid - corrected pion and kaon yields @xmath26 .\n",
            "first proposed by collins , heppelman and ladinsky  @xcite , the iff describes the fragmentation of a polarized quark into two hadrons correlated via partial wave interference .\n",
            "this approach is not susceptible to qcd radiative effects and the @xmath43 azimuthal modulation @xmath44 is directly proportional to the product of two iff @xmath45 , where @xmath46 represents the fractional energy of the hadron pair and @xmath47 its invariant mass .\n",
            "154\n",
            "154\n",
            "1433\n",
            "133\n",
            "abstract\n",
            "these days it is common for young operator algebraists to know a lot about c@xmath0-algebras , or a lot about von neumann algebras  but not both . though a natural consequence of the breadth and depth of each subject , this is unfortunate as the interplay between the two theories has deep historical roots and has led to many beautiful results . \n",
            " we review some of these connections , in the context of amenability , with the hope of convincing ( younger ) readers that tribalism impedes progress .\n",
            "89\n",
            "13650\n",
            "Lex Rank Summary\n",
            "a _ @xmath49-norm _  @xmath70 on @xmath71 is a norm such that @xmath72 , @xmath73 and @xmath74 for all @xmath75  .\n",
            "is a c.c.p .\n",
            "but we re about to come full circle and use this result to prove ozawa s solidity theorem for von neumann algebras , so it s a bit misleading to say that ozawa s work is an application of c@xmath0-theory to w@xmath0-algebras .\n",
            "hence we have a canonical action of @xmath219 on @xmath391 which we ll denote by @xmath394 for all @xmath232 and @xmath395 .\n",
            "see theorem 4.3.4 and lemma 4.3.7 in @xcite for a proof of the following fact .\n",
            "102\n",
            "102\n",
            "13650\n",
            "89\n",
            "abstract\n",
            "we determine the size of the elementary quasihole in @xmath0 and @xmath1 quantum hall states via exact - diagonalization and density - matrix renormalization group calculations on the sphere and cylinder , using a variety of short- and long - range pinning potentials . \n",
            " the size of the quasihole at filling factor @xmath0 is estimated to be @xmath2 , and that of @xmath1 is @xmath3 , where @xmath4 is the magnetic length . \n",
            " in contrast , the size of the laughlin quasihole , expected to capture the basic physics in these two states , is around @xmath5 . \n",
            " our work supports the earlier findings that the quasihole in the first excited landau level is significantly larger than in the lowest landau level .\n",
            "123\n",
            "4551\n",
            "Lex Rank Summary\n",
            "in the present work we consider a finite quantum hall system on the surface of a sphere  @xcite or a cylinder  @xcite .\n",
            "to characterize the spatial extent of the quasihole defect , we compute the  excess charge \" ( integrated deviation of the density from the background density of the ground state ) @xmath27 here @xmath28 is the density of the quasihole state at the spherical angle @xmath29  , @xmath30 is the density of the ground state ( a trivial constant on the sphere ) , and the integral is over the unit sphere ( @xmath31 as a function of distance @xmath32 in physical units is obtained by simple rescaling with @xmath33 at the end ) .\n",
            "in order to find the ground state of the hamiltonian , we use exact diagonalization , as well as density - matrix renormalization ( dmrg ) group  @xcite ( for details of our dmrg implementation , see ref .  )\n",
            "state on the sphere .\n",
            "in fig .\n",
            "162\n",
            "162\n",
            "4551\n",
            "123\n",
            "abstract\n",
            "the study of young stars no longer surrounded by disks can greatly add to our understanding of how protoplanetary disks evolve and planets form . \n",
            " we have used vlt / flames optical spectroscopy to confirm the youth and membership of 19 new young diskless stars in the serpens molecular cloud , identified at x - ray wavelengths . \n",
            " spectral types , effective temperatures and stellar luminosities were determined using the optical spectra and optical / near - ir photometry . \n",
            " stellar masses and ages were derived based on pms evolutionary tracks . \n",
            " the results yield remarkable similarities for age and mass distribution between the diskless and disk - bearing stellar populations in serpens . \n",
            " we discuss the important implications these similarities may have on the standard picture of disk evolution .\n",
            "131\n",
            "8714\n",
            "Lex Rank Summary\n",
            "indeed , x - ray emission has been often used to identify young stellar objects in the literature ( e.g. @xcite ) .\n",
            "a larger uncertainty is found for the spectra with lower s / n .  the distribution of spectral types from this work is shown in figure [ f_spt ] , while the results for individual stars can be found in table [ t_spt ] .\n",
            "it is worth noting that the spectra of objects 02 - 005 and 02 - 025 do not show li i , while the line is seen in the spectra of 02 - 008 and 02 - 039 . at this point  it is difficult to confirm membership and these four objects are left out of the further discussion .\n",
            "the most straightforward explanation for why the disks around these newly confirmed young stars have already dissipated would be that these stars are systematically a few myr older than the stars with disks in the same area of serpens @xcite .\n",
            "that is not to say that either parameter is not important for disk evolution : the big picture remains that disks evolve with time and , statistically , older stars have more evolved ( or no ) disks compared to young stars .\n",
            "208\n",
            "208\n",
            "8714\n",
            "131\n",
            "abstract\n",
            "we investigate here the spectrum of gravitational collapse endstates when arbitrarily small perfect fluid pressures are introduced in the classic black hole formation scenario as described by oppenheimer , snyder and datt ( osd ) @xcite . \n",
            " this extends a previous result on tangential pressures @xcite to the more physically realistic scenario of perfect fluid collapse . \n",
            " the existence of classes of pressure perturbations is shown explicitly , which has the property that injecting any smallest pressure changes the final fate of the dynamical collapse from a black hole to a naked singularity . \n",
            " it is therefore seen that any smallest neighborhood of the osd model , in the space of initial data , contains collapse evolutions that go to a naked singularity outcome . \n",
            " this gives an intriguing insight on the nature of naked singularity formation in gravitational collapse .\n",
            "141\n",
            "4876\n",
            "Lex Rank Summary\n",
            "actually from the many dynamical gravitational collapse scenarios that have been investigated over the past years , the typical conclusion that has emerged is as follows : depending on the nature of the initial data for the matter cloud in terms of its initial density , pressure and velocity profiles from which the collapse evolves , there are dynamical evolutions governed by the einstein equations that take the collapse to either a black hole or naked singularity final state ( see e.g. @xcite and references therein ) .\n",
            "we show explicitly the existence of classes of small generic pressure perturbations such that an injection of a small positive ( or negative ) pressure in the osd model , or in a tolman - bondi - lemaitre ( tbl ) inhomogeneous dust collapse to a black hole @xcite , leads the collapse to form a naked singularity , rather than a black hole .\n",
            "in a neighborhood of the center  this is given by , @xmath28 the quantity @xmath29 is the tangent to the singularity curve at the origin , and if it has a positive value then the singularity turns out to be naked , while otherwise it would be hidden in a black hole .\n",
            "we consider an explicit class of perfect fluid collapse models by introducing a small pressure to the tbl scenario , to solve einstein equations in a neighborhood of the center .\n",
            "we therefore see that it is always possible to find a suitable positive pressure perturbation of the osd collapse model that , however small , will cause the collapse to end in a naked singularity .\n",
            "269\n",
            "269\n",
            "4876\n",
            "141\n",
            "abstract\n",
            "five - dimensional black holes are studied in lovelock gravity coupled to hoffmann - infeld non - linear electrodynamics . \n",
            " it is shown that some of these solutions present a double peak behavior of the temperature as a function of the horizon radius . \n",
            " this feature suggests that the evaporation process , though drastic for a period , leads to an eternal black hole remnant . \n",
            " in fact , the form of the caloric curve corresponds to the existence of a _ plateau _ in the evaporation rate , which implies that black holes of intermediate scales turn out to be unstable . \n",
            " the geometrical aspects , such as the absence of conical singularity , the structure of horizons , etc . are also discussed . in particular , solutions that are \n",
            " asymptotically ads arise for special choices of the parameters , corresponding to charged solutions of five - dimensional chern - simons gravity .\n",
            "155\n",
            "3524\n",
            "Lex Rank Summary\n",
            "typically , this particular behavior leads to the presence of a _ plateau _ in the evaporation rate , implying a drastic evaporation for those black holes having sizes which are bounded between the two scales where the peaks are located .\n",
            "moreover , by comparing the solution ( [ sol ] ) and the one corresponding to the lovelock - born - infeld black holes @xcite , it is feasible to verify that in both theories @xmath75 can be set to @xmath76 at the origin @xmath61 .\n",
            "nevertheless , in the case of lovelock - hoffmann - infeld solutions , we find that @xmath77 vanishes in the limit @xmath78 whereas it goes to @xmath79 for lovelock - born - infeld black holes ( see fig .\n",
            "certainly , it is known that black holes in lovelock gravity present special features which are not shared with their analogues in einstein gravity theory ; namely , these black holes typically have an infinite lifetime , present a positive specific heat for small radii , their isotermal graphs for the charged cases turn out to be rather different @xcite , violate the bekenstein s area formula @xcite and the temperature formula in the general case presents an additional term which identically vanishes for @xmath80 .\n",
            "[ fig1a ] and [ temp3 ] .\n",
            "217\n",
            "217\n",
            "3524\n",
            "155\n",
            "abstract\n",
            "recent observations of accreting black holes reveal the presence of quasi - periodic oscillations ( qpo ) in the optical power density spectra . \n",
            " the corresponding oscillation periods match those found in the x - rays , implying a common origin . among the numerous suggested x - ray qpo mechanisms , \n",
            " some may also work in the optical . \n",
            " however , their relevance to the broadband \n",
            " optical through x - ray  spectral properties have not been investigated . \n",
            " for the first time , we discuss the qpo mechanism in the context of the self - consistent spectral model . \n",
            " we propose that the qpos are produced by lense - thirring precession of the hot accretion flow , whose outer parts radiate in the optical wavelengths . at the same time , its innermost parts are emitting the x - rays , explaining the observed connection of qpo periods . \n",
            " we predict that the x - ray and optical qpos should be either in phase or shifted by half a period , depending on the observer position . \n",
            " we investigate the qpo harmonic content and find that the variability amplitudes at the fundamental frequency are larger in the optical , while the x - rays are expected to have strong harmonics . \n",
            " we then discuss the qpo spectral dependence and compare the expectations to the existing data .\n",
            "228\n",
            "6514\n",
            "Lex Rank Summary\n",
            "in section  [ sect : models_setup ] we develop a quantitative model for the low - frequency oir and x - ray qpos , which are produced by lense - thirring precession of a hot accretion flow .\n",
            "the specific flux observed far from the bh from a ring of thickness @xmath44 at radius @xmath45 in the direction that makes an angle @xmath46 to the surface normal can be expressed as @xmath47 here , @xmath48 is the distance to the observer , @xmath49 is the surface flux per energy interval at a given radius and the factor @xmath50 accounts for the angular dependence of the observed flux .\n",
            "this can also be seen in the ( quasi- ) simultaneous data of @xcite , where both optical and x - ray psds show a qpo at @xmath91  hz , two harmonics @xmath92  hz and @xmath93  hz are seen in the x - ray , but not in the optical psd .\n",
            "in figure  [ fig : qpo_freq ] we reproduced the range of possible qpo frequencies ( the same for optical and x - rays ) as a function of the hot flow outer radius .\n",
            "here  we show that the x - ray qpos should have smaller rms at the fundamental frequency than the oir qpos .\n",
            "213\n",
            "213\n",
            "6514\n",
            "228\n",
            "abstract\n",
            "we consider a simple but important class of metastable discrete time markov chains , which we call perturbed markov chains . \n",
            " basically , we assume that the transition matrices depend on a parameter @xmath0 , and converge as @xmath1 . \n",
            " we further assume that the chain is irreducible for @xmath2 but may have several essential communicating classes when @xmath3 . \n",
            " this leads to metastable behavior , possibly on multiple time scales . for each of the relevant time scales , \n",
            " we derive two effective chains . \n",
            " the first one describes the ( possibly irreversible ) metastable dynamics , while the second one is reversible and describes metastable escape probabilities . \n",
            " closed probabilistic expressions are given for the asymptotic transition probabilities of these chains , but we also show how to compute them in a fast and numerically stable way . as a consequence , \n",
            " we obtain efficient algorithms for computing the committor function and the limiting stationary distribution . \n",
            " escape times , non - reversible markov chains , asymptotics     60j10 , 60j22\n",
            "172\n",
            "13035\n",
            "Lex Rank Summary\n",
            "in this paper we give a detailed analysis of the asymptotic dynamics and stationary distribution for a special class of metastable markov chains .\n",
            "for all @xmath130 with @xmath142 , and all @xmath22 .\n",
            "in the case of perturbed markov chains on a finite state space , definition 2.1 from @xcite ( see also @xcite ) goes as follows : a set @xmath316 is called a _ set of metastable points _ if for all @xmath317 and @xmath318 , [ bovier def ] _ 0 = 0 . in words  , this means that reaching @xmath319 from the outside of @xmath319 is much easier than traveling between different points of @xmath319 , in both cases with the restriction not to return to one s starting point first .\n",
            "it follows that @xmath32 is in the same @xmath519-essential class as @xmath201 , and thus not a @xmath519-transient state .\n",
            "when a markov chain is nearly reducible , it is known ( and follows from in our case ) that we can ignore transitions between different @xmath556 for the approximate computation of the @xmath557 ; in the case of perturbed markov chains and when each @xmath556 contains exactly one @xmath204-essential class @xmath502 , this means @xmath570 .\n",
            "201\n",
            "201\n",
            "13035\n",
            "172\n",
            "abstract\n",
            "we show that using mid - ir color selection to find active galactic nuclei ( agns ) is as effective in dense stellar fields such as the magellanic clouds as it is in extragalactic fields with low stellar densities using comparisons between the _ spitzer _ deep , wide - field survey data for the noao deep wide field survey botes region and the sage survey of the large magellanic cloud . \n",
            " we use this to build high purity catalogs of @xmath0 agn candidates behind the magellanic clouds . \n",
            " once confirmed , these quasars will expand the available astrometric reference sources for the clouds and the numbers of quasars with densely sampled , long - term ( @xmath1decade ) monitoring light curves by well over an order of magnitude and potentially identify sufficiently bright quasars for absorption line studies of the interstellar medium of the clouds .\n",
            "147\n",
            "4268\n",
            "Lex Rank Summary\n",
            "because of the microlensing studies of the magellanic clouds and the galactic bulge ( eros  ; macho  @xcite ; moa  @xcite ; ogle  @xcite ) , most quasars identified in these regions will have well - sampled , decade long light curves that can be used to study the optical variability of quasars .\n",
            "we use this method to produce a catalog of 4699 , and 657 quasar candidates in the lmc and smc based on the sage ( @xcite ) and s3mc ( @xcite ) surveys .\n",
            "we matched the sage sources with the ogle - iii optical photometry for their region of overlap , and in figure  [ fig : optical - ir ] we examine the @xmath13$]/@xmath6-[8.0]$ ] color - color distribution of the botes quasars as compared to our qso - a , qso - b , yso - a and yso - b sources as well as the `` high probability '' yso candidates from whitney et al .  we divide this color space into region `` a '' containing the botes quasars and region `` b '' outside of it .\n",
            "a quasar candidate is any object other than class c objects from cut 1 and `` other '' objects from cut 2 . for the botes quasars , 6,599/608 are class a / b , 6,131/11 are qso / yso , and 5,961/181 are class a / b .  stellar contamination will be higher for class b , yso and b than for class a , qso and a. of the 722 whitney et al .  ( 2008 ) yso candidates , 478 are in the agn wedge and , of these , 184 ( 191 ) lie in the qso ( yso ) regions .\n",
            "the purity of our sample compared to a similar extragalactic search will be very high in the primary qso - a region , poorer if searching for the brightest quasars in the yso - a region , and very poor in the qso / yso - b regions where the color locus of black bodies crosses the @xcite color selection region .\n",
            "351\n",
            "351\n",
            "4268\n",
            "147\n",
            "abstract\n",
            "combinations of oscillations with incommensurate periods are utilized to generate discrete planar structures with non - crystallographic symmetries . \n",
            " some previously known tilings and results are reconsidered in this context . a new kind of decagonal tiling , its relations with the penrose tilings and some experimental reports are discussed .\n",
            "51\n",
            "3183\n",
            "Lex Rank Summary\n",
            "the eightfold case can be also reproduced with this method but it has been already been exposed at some length in a study developing a somewhat similar approach@xcite .\n",
            "it has been obtained by retaining just two terms with equal amplitudes and @xmath26 and @xmath27 , where @xmath28 which is the golden mean , and @xmath29 .\n",
            "retaining only the most regular elements of this structure , it is possible to devise a geometrical reconstruction as the one shown in fig.2 .\n",
            "it appears that such tilings can be obtained with a single figure when some rules are observed .\n",
            "a pentagon can be cut from either side of the hexagons in sdt and if this is performed in a disordered way , when crowns are reunited with other elements , a variant of the random pentagonal penrose tiling @xcite would be produced .\n",
            "140\n",
            "140\n",
            "3183\n",
            "51\n",
            "abstract\n",
            "we consider close - packed dimers , or perfect matchings , on two - dimensional regular lattices . \n",
            " we review known results and derive new expressions for the free energy , entropy , and the molecular freedom of dimers for a number of lattices including the simple - quartic @xmath0 , honeycomb @xmath1 , triangular @xmath2 , kagom @xmath3 , 3 - 12 @xmath4 and its dual @xmath5 $ ] , and 4 - 8 @xmath6 and its dual union jack @xmath7 $ ] archimedean tilings . \n",
            " the occurrence and nature of phase transitions are also analyzed and discussed . \n",
            " * key words : * close - packed dimers , two - dimensional lattices , exact results , phase transitions .\n",
            "121\n",
            "3981\n",
            "Lex Rank Summary\n",
            "here we review known results and derive new expressions for the free energy , entropy , and molecular freedom for various archimedean two - dimensional lattices .\n",
            "for a simple - quartic lattice with uniform dimer weights @xmath22 and @xmath23 in the two ( horizontal and vertical ) directions , we have @xcite - @xcite ( see also section 4 below ) f_sq(z_1,z_2 ) = 1 8 ^ 2 _ 0 ^ 2 d_0 ^ 2 d . [ square ]  the free energy @xmath24 is regular in @xmath22 and @xmath23 .\n",
            "the checkerboard lattice is a simple - quartic lattice with anisotropic dimer weights @xmath27 and @xmath34 as shown in fig .\n",
            "1 is the @xmath37-direction . ]\n",
            "[ sqmatrix ] explicitly , this leads to & & f_ckb(z_1,z_2,z_3,z_4 ) = 1 8 ^ 2 _ 0 ^ 2 d_0 ^ 2 d | z_1-iz_4e^i + iz_2 e^i -z_3 e^i(+ ) |^2 + & = & 1 8 ^ 2 _ 0 ^ 2 d_0 ^ 2 d  .  [ ckd ] for @xmath38 the solution reduces to ( [ square ] ) for the simple - quartic lattice with uniform weights , and for @xmath39 the solution reduces to ( [ honeycomb ] ) for the honeycomb lattice .\n",
            "207\n",
            "207\n",
            "3981\n",
            "121\n",
            "abstract\n",
            "we derive an _ ab initio _ @xmath0-band tight - binding model for @xmath1 stacked bilayer graphene based on maximally localized wannier wave functions ( mlwfs ) centered on the carbon sites , finding that both intralayer and interlayer hopping is longer in range than assumed in commonly used phenomenological tight - binding models . starting from this full tight - binding model , \n",
            " we derive two effective models that are intended to provide a convenient starting point for theories of @xmath0-band electronic properties by achieving accuracy over the full width of the @xmath0-bands , and especially at the dirac points , in models with a relatively small number of hopping parameters . \n",
            " the simplified models are then compared with phenomenological slonczewski - weiss - mcclure type tight - binding models in an effort to clarify confusions that exists in the literature concerning tight - binding model parameter signs .\n",
            "150\n",
            "4041\n",
            "Lex Rank Summary\n",
            "in the main text  we quantify the role they play in bilayer graphene electronic structure.,width=279 ]  a @xmath0-band model of bilayer graphene contains four orthogonal orbitals per unit cell , corresponding to @xmath9 orbitals centered on the @xmath7 , @xmath6 sites in the bottom layer and @xmath10 and @xmath11 sites in the top layer .\n",
            "the swm model for a bilayer graphene  is simplified because @xmath83 and the absence of the dispersion along the @xmath84-axis resulting in the hamiltoinan @xmath85 where for a bilayer graphene @xmath86 we have @xmath87 where @xmath88 with @xmath63 measured from the dirac point and @xmath89 is the angle measured from the @xmath90 axis .\n",
            "comparing with the four eigenvalues of the tight - binding hamiltonian we can conclude that @xmath95 the eigenvalues along the @xmath96 line from the swm bilayer graphene model are given by @xmath97 where @xmath98    this is to be compared with the four eigenvalues of the effective continuum model whose eigenvalues are @xmath99 where @xmath100 when we compare the eqs .\n",
            "b 77 , 041407(r ) ( 2008 ) ; f. zhang , j. jung , g. a. fiete , q. niu , and a. h. macdonald , phys .\n",
            "rev  109 , 126402 ( 2012 ) ; f. zhang , h. min , and a. h. macdonald , phys .\n",
            "215\n",
            "215\n",
            "4041\n",
            "150\n",
            "abstract\n",
            "a construction of node - less atomic orbitals and energy - dependent , node - reduced partial waves is presented , that contains the full information of the atomic eigenstates and that allows to represent the scattering properties in a transparent manner . by inverting the defining schrdinger equation , \n",
            " the pauli repulsion by the core electrons can be represented as effective potential . \n",
            " this construction also provides a description of the pauli repulsion by an environment . \n",
            " furthermore , the representation leads to a new systematic scheme for a projector augmentation . \n",
            " the relation to slater orbitals is discussed .\n",
            "101\n",
            "4622\n",
            "Lex Rank Summary\n",
            "[ eq : defq ] with eq .\n",
            "[ eq : nodelessbound ] , we obtain that the bound states of the node - reduced partial waves are the node - less wave functions defined before , i.e. @xmath25    the energy - dependent wave function @xmath0 can be reconstructed from the node - reduced wave function @xmath26 and the node - less bound states @xmath14 by @xmath27 \\nonumber\\\\ & & \\times \\prod_{j=1}^{n-1}(e_j - e)\\;.\n",
            "[ eq : ansatzphi ] into eq .\n",
            "[ eq : defq ] and boundary conditions eq .\n",
            "[ eq : defq ] and [ eq : qofen ] for the node - reduced functions @xmath91 , we find @xmath94 which is identical to the differential equation eq .\n",
            "119\n",
            "119\n",
            "4622\n",
            "101\n",
            "abstract\n",
            "the first detection of co emission in a fanaroff - riley class ii ( i.e. , edge - brightened radio morphology ) radio galaxy is presented . \n",
            " multiwavelength ( 0.36 - 2.17 @xmath0 m ) imaging of 3c 293 shows it to be a disk galaxy with an optical jet or tidal tail extending towards what appears to be a companion galaxy 28 kpc away via a low surface brightness envelope . the molecular gas appears to be distributed in an asymmetric disk rotating around an unresolved continuum source , which is presumably emission from the agn . a narrow ( @xmath1 km s@xmath2 ) absorption feature \n",
            " is also observed in the co spectrum and is coincident with the continuum source . using the standard co conversion factor , \n",
            " the molecular gas ( h@xmath3 ) mass is calculated to be 1.5@xmath4 m@xmath5 , several times the molecular gas mass of the milky way . \n",
            " the high concentration of molecular gas within the central 3 kpc of 3c 293 , combined with the multiwavelength morphological peculiarities , support the idea that the radio activity has been triggered by a gas - rich galaxy - galaxy interaction or merger event .\n",
            "199\n",
            "6289\n",
            "Lex Rank Summary\n",
            "section 2 is a discussion of the optical , near - infrared , and millimeter observations of 3c 293 .  the data reduction methods and molecular gas mass calculations are summarized in  3 .  section 4 contains an estimate of the dynamical mass of 3c 293 based on the co data , a discussion of the 2.7 mm continuum emission and co absorption , and concludes with a detailed comparison of the morphologies of the galaxy at optical , near - infrared , millimeter , and radio wavelengths .\n",
            "given that the standard gas - to - dust ratio is 100200 , and that the 2.7 mm continuum emission is not spatially extended like the co emission , the 2.7 mm continuum emission is unlikely to be thermal emission emanating from dust associated with the molecular gas .\n",
            "the elliptical galaxy ngc 3377 , believed to harbor a @xmath95 m@xmath60 black hole , has a velocity dispersion of 90 km s@xmath2 which increases to @xmath96 km s@xmath2 within the central 1@xmath11 ( 48 pc : kormendy et al .  however , if the dynamical mass within the inner 2.8 kpc of 3c 293 is on the order of @xmath97 m@xmath60 , 3c 293 as a whole may have a mass comparable to a massive elliptical galaxy ( @xmath98 m@xmath60 ) .\n",
            "however , the companion appears to be a galaxy and not a foreground star ; the measured fwhm of the companion in the 2.17 @xmath105 image is 2.1@xmath11 , as compared with 1.2@xmath11 for stars in the field .\n",
            "this , and the fact that the continuum emission is not coincident with the co emission , indicates that the 2.7 mm continuum emission is nonthermal in nature , and that it most likely emanates from a circumnuclear accretion disk around a supermassive black hole , and not from dust associated with the molecular gas .\n",
            "312\n",
            "312\n",
            "6289\n",
            "199\n",
            "abstract\n",
            "we analyse various phonon - assisted mechanisms which contribute to the decoherence of excitonic qubits in quantum dot systems coupled by the frster - type transfer process . \n",
            " we show the significant loss of coherence accompanied by dissipation due to charge carrier oscillations between qubit states by using a model of one - phonon assisted frster - type transfer process . \n",
            " we obtain explicit expressions for the relaxation and dephasing times for excitonic qubits interacting with acoustic phonons via both deformation potential and piezoelectric coupling . \n",
            " we compare the decoherence times of the gaas / algaas material system with half times of concurrence decay in a 2@xmath02 bipartite mixed excitonic qubit system . \n",
            " we extend calculations to determine the influence of phonon mediated interactions on the non - unitary evolution of berry phase in quantum dot systems .\n",
            "138\n",
            "7355\n",
            "Lex Rank Summary\n",
            "@xmath12 in eq .\n",
            "@xmath50 is the difference in exciton creation energy between the quantum dot at @xmath1 and that at @xmath2 .\n",
            "[ eq : anfactorta1 ] and [ eq : anfactorta2 ] .\n",
            "[ eq : pathphase1 ] - [ eq : pathphase4 ] .\n",
            "[ eq : gfun2 ] ) and the functions @xmath229 and @xmath225 are given by @xmath230 where @xmath231 can be obtained using eqs .\n",
            "67\n",
            "67\n",
            "7355\n",
            "138\n",
            "abstract\n",
            "we present a study of the scaling properties of cluster - cluster aggregation with a source of monomers in the stationary state when the spatial transport of particles occurs by lvy flights . \n",
            " we show that the transition from mean - field statistics to fluctuation - dominated statistics which , for the more commonly considered case of diffusive transport , occurs as the spatial dimension of the system is tuned through two from above , can be mimicked even in one dimension by varying the characteristic exponent , @xmath0 , of the the lvy jump length distribution . \n",
            " we also show that the two - point mass correlation function , responsible for the flux of mass in the stationary state , is strongly universal : its scaling exponent is given by the mean field value independent of the spatial dimension and independent of the value of @xmath0 . \n",
            " finally we study numerically the two point spatial correlation function which characterises the structure of the depletion zone around heavy particles in the diffusion limited regime . \n",
            " we find that this correlation function vanishes with a non - trivial fractional power of the separation between particles as this separation goes to zero . \n",
            " we provide a scaling argument for the value of this exponent which is in reasonable agreement with the numerical measurements . \n",
            " citation : c connaughton and j harris j. stat . \n",
            " mech . \n",
            " ( 2010 ) p05003    doi : 10.1088/1742 - 5468/2010/05/p05003\n",
            "243\n",
            "7688\n",
            "Lex Rank Summary\n",
            "that is to say that if the density has a scaling exponent , @xmath38 , then the corresponding scaling exponent of an order @xmath39 correlation function is @xmath40 .\n",
            "such hops are referred to as lvy _ flights _  @xcite and should not be confused with the ( often more physically realistic ) case of lvy _ walks _ in which the waiting time distribution and the jump length distribution are not independent to account for the fact that for particles of finite mass long jumps should take more time .\n",
            "in eq .\n",
            "in the case of stationary cca with lvy flights ,  the anomalous diffusion length for particles of mass @xmath2 in one dimension is , dimensionally , @xmath127 the fact that the correlation between particles vanishes linearly in the case of regular diffusion follows from the calculations performed in @xcite and is connected to the fact that the spatial transport mechanism is diffusion .\n",
            "( [ eq - aa2a ] ) or eq .\n",
            "163\n",
            "163\n",
            "7688\n",
            "243\n",
            "abstract\n",
            "the gauge invariant non local quantum dynamics of the aharonov - bohm effect can be tested experimentally by measuring the instantaneous shift of the velocity distribution occurring when the particle passes by the flux line . \n",
            " it is shown that in relativistic quantum theory it is possible to measure the instantaneous velocity with accuracy sufficient to detect the change of the velocity distribution . in non relativistic quantum theory \n",
            " the instantaneous velocity can be measured to any desired accuracy . \n",
            " +   + pacs 03.65.ta , 06.30.gv    @xmath0__school of physics and astronomy , tel aviv university , tel aviv 69978 , israel _ _ + @xmath1__e - mail : trka@post.tau.ac.il__\n",
            "109\n",
            "3715\n",
            "Lex Rank Summary\n",
            "since a measurement of velocity  does not change the velocity , an observed shift of the velocity distribution will attest that the change existed prior to the measurement , i.e. , shortly after the wave packets passed by the flux line .\n",
            "[ [ section-1 ] ]    after a brief introduction of von neumann s theory , its application to the measurement of position@xmath8 and to the measurement of velocity@xmath9 , the measurement of velocity by means of two position measurements is described@xmath10 .\n",
            "thus , the measurement of velocity involves the hamiltonian @xmath54 where the gate function is defined by @xmath55 for @xmath56 , @xmath57 for @xmath58 , @xmath59 for @xmath60 and @xmath61 otherwise .\n",
            "thus , with a measurement of the particle s velocity , we have to expand its state in eigenstates of velocity , @xmath128 where @xmath129 , @xmath130 , are the fourier transforms of the wave functions @xmath131 and @xmath132 , respectively@xcite .\n",
            "[ [ section-9 ] ]    note that in the case when there is a relative velocity between the wave packets , as with the superposition @xmath143 $ ] , the velocity distributions of the two wave packets do not overlap and no shift of the velocity distribution is observed .\n",
            "204\n",
            "204\n",
            "3715\n",
            "109\n",
            "HELLO\n"
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              "                                              Summary  \\\n",
              "0   however , for simplicity , the disk emissivity...   \n",
              "1   the leading scenarios for the origin of short ...   \n",
              "2   inside the hybrid star  , one has only to cons...   \n",
              "3   imaging is therefore limited to 35  at the 2.2...   \n",
              "4   the cool giant can also show intrinsic variabi...   \n",
              "..                                                ...   \n",
              "95  [ eq : defq ] with eq .[ eq : nodelessbound ] ...   \n",
              "96  section 2 is a discussion of the optical , nea...   \n",
              "97  @xmath12 in eq .@xmath50 is the difference in ...   \n",
              "98  that is to say that if the density has a scali...   \n",
              "99  since a measurement of velocity  does not chan...   \n",
              "\n",
              "                                              Article  \\\n",
              "0   with the discovery of fe  k@xmath0  emission a...   \n",
              "1   gamma ray bursts ( grbs ) divide into two dist...   \n",
              "2   neutron stars must be one of the most suitable...   \n",
              "3   the _ reuven ramaty high energy solar spectros...   \n",
              "4   most stars in the universe are binaries . amon...   \n",
              "..                                                ...   \n",
              "95  first - principles electronic - structure calc...   \n",
              "96  there exists substantial evidence that galaxy ...   \n",
              "97  the use of excitons ( electron - hole correlat...   \n",
              "98  cluster - cluster aggregation ( cca ) refers t...   \n",
              "99  in a previous article@xcite it has been shown ...   \n",
              "\n",
              "                                             Abstract  Summary Length  \\\n",
              "0   in this paper , we present a simple relativist...             271   \n",
              "1   the first well - localized short - duration ga...             427   \n",
              "2   we estimate the critical magnetic field streng...             227   \n",
              "3   the reuven ramaty high energy solar spectrosco...             260   \n",
              "4   symbiotic stars are long - period interacting ...             297   \n",
              "..                                                ...             ...   \n",
              "95  a construction of node - less atomic orbitals ...             119   \n",
              "96  the first detection of co emission in a fanaro...             312   \n",
              "97  we analyse various phonon - assisted mechanism...              67   \n",
              "98  we present a study of the scaling properties o...             163   \n",
              "99  the gauge invariant non local quantum dynamics...             204   \n",
              "\n",
              "    Article Length  Abstract Length  \n",
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              "      <td>inside the hybrid star  , one has only to cons...</td>\n",
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              "      <td>we estimate the critical magnetic field streng...</td>\n",
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              "      <td>143</td>\n",
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              "      <td>the _ reuven ramaty high energy solar spectros...</td>\n",
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              "      <td>section 2 is a discussion of the optical , nea...</td>\n",
              "      <td>there exists substantial evidence that galaxy ...</td>\n",
              "      <td>the first detection of co emission in a fanaro...</td>\n",
              "      <td>312</td>\n",
              "      <td>6289</td>\n",
              "      <td>199</td>\n",
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              "      <th>97</th>\n",
              "      <td>@xmath12 in eq .@xmath50 is the difference in ...</td>\n",
              "      <td>the use of excitons ( electron - hole correlat...</td>\n",
              "      <td>we analyse various phonon - assisted mechanism...</td>\n",
              "      <td>67</td>\n",
              "      <td>7355</td>\n",
              "      <td>138</td>\n",
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              "    <tr>\n",
              "      <th>98</th>\n",
              "      <td>that is to say that if the density has a scali...</td>\n",
              "      <td>cluster - cluster aggregation ( cca ) refers t...</td>\n",
              "      <td>we present a study of the scaling properties o...</td>\n",
              "      <td>163</td>\n",
              "      <td>7688</td>\n",
              "      <td>243</td>\n",
              "    </tr>\n",
              "    <tr>\n",
              "      <th>99</th>\n",
              "      <td>since a measurement of velocity  does not chan...</td>\n",
              "      <td>in a previous article@xcite it has been shown ...</td>\n",
              "      <td>the gauge invariant non local quantum dynamics...</td>\n",
              "      <td>204</td>\n",
              "      <td>3715</td>\n",
              "      <td>109</td>\n",
              "    </tr>\n",
              "  </tbody>\n",
              "</table>\n",
              "<p>100 rows × 6 columns</p>\n",
              "</div>\n",
              "      <button class=\"colab-df-convert\" onclick=\"convertToInteractive('df-80999795-6013-4191-8098-8419ea4f195b')\"\n",
              "              title=\"Convert this dataframe to an interactive table.\"\n",
              "              style=\"display:none;\">\n",
              "        \n",
              "  <svg xmlns=\"http://www.w3.org/2000/svg\" height=\"24px\"viewBox=\"0 0 24 24\"\n",
              "       width=\"24px\">\n",
              "    <path d=\"M0 0h24v24H0V0z\" fill=\"none\"/>\n",
              "    <path d=\"M18.56 5.44l.94 2.06.94-2.06 2.06-.94-2.06-.94-.94-2.06-.94 2.06-2.06.94zm-11 1L8.5 8.5l.94-2.06 2.06-.94-2.06-.94L8.5 2.5l-.94 2.06-2.06.94zm10 10l.94 2.06.94-2.06 2.06-.94-2.06-.94-.94-2.06-.94 2.06-2.06.94z\"/><path d=\"M17.41 7.96l-1.37-1.37c-.4-.4-.92-.59-1.43-.59-.52 0-1.04.2-1.43.59L10.3 9.45l-7.72 7.72c-.78.78-.78 2.05 0 2.83L4 21.41c.39.39.9.59 1.41.59.51 0 1.02-.2 1.41-.59l7.78-7.78 2.81-2.81c.8-.78.8-2.07 0-2.86zM5.41 20L4 18.59l7.72-7.72 1.47 1.35L5.41 20z\"/>\n",
              "  </svg>\n",
              "      </button>\n",
              "      \n",
              "  <style>\n",
              "    .colab-df-container {\n",
              "      display:flex;\n",
              "      flex-wrap:wrap;\n",
              "      gap: 12px;\n",
              "    }\n",
              "\n",
              "    .colab-df-convert {\n",
              "      background-color: #E8F0FE;\n",
              "      border: none;\n",
              "      border-radius: 50%;\n",
              "      cursor: pointer;\n",
              "      display: none;\n",
              "      fill: #1967D2;\n",
              "      height: 32px;\n",
              "      padding: 0 0 0 0;\n",
              "      width: 32px;\n",
              "    }\n",
              "\n",
              "    .colab-df-convert:hover {\n",
              "      background-color: #E2EBFA;\n",
              "      box-shadow: 0px 1px 2px rgba(60, 64, 67, 0.3), 0px 1px 3px 1px rgba(60, 64, 67, 0.15);\n",
              "      fill: #174EA6;\n",
              "    }\n",
              "\n",
              "    [theme=dark] .colab-df-convert {\n",
              "      background-color: #3B4455;\n",
              "      fill: #D2E3FC;\n",
              "    }\n",
              "\n",
              "    [theme=dark] .colab-df-convert:hover {\n",
              "      background-color: #434B5C;\n",
              "      box-shadow: 0px 1px 3px 1px rgba(0, 0, 0, 0.15);\n",
              "      filter: drop-shadow(0px 1px 2px rgba(0, 0, 0, 0.3));\n",
              "      fill: #FFFFFF;\n",
              "    }\n",
              "  </style>\n",
              "\n",
              "      <script>\n",
              "        const buttonEl =\n",
              "          document.querySelector('#df-80999795-6013-4191-8098-8419ea4f195b button.colab-df-convert');\n",
              "        buttonEl.style.display =\n",
              "          google.colab.kernel.accessAllowed ? 'block' : 'none';\n",
              "\n",
              "        async function convertToInteractive(key) {\n",
              "          const element = document.querySelector('#df-80999795-6013-4191-8098-8419ea4f195b');\n",
              "          const dataTable =\n",
              "            await google.colab.kernel.invokeFunction('convertToInteractive',\n",
              "                                                     [key], {});\n",
              "          if (!dataTable) return;\n",
              "\n",
              "          const docLinkHtml = 'Like what you see? Visit the ' +\n",
              "            '<a target=\"_blank\" href=https://colab.research.google.com/notebooks/data_table.ipynb>data table notebook</a>'\n",
              "            + ' to learn more about interactive tables.';\n",
              "          element.innerHTML = '';\n",
              "          dataTable['output_type'] = 'display_data';\n",
              "          await google.colab.output.renderOutput(dataTable, element);\n",
              "          const docLink = document.createElement('div');\n",
              "          docLink.innerHTML = docLinkHtml;\n",
              "          element.appendChild(docLink);\n",
              "        }\n",
              "      </script>\n",
              "    </div>\n",
              "  </div>\n",
              "  "
            ]
          },
          "metadata": {},
          "execution_count": 10
        }
      ]
    },
    {
      "cell_type": "code",
      "source": [
        "print(baseline_rouge)"
      ],
      "metadata": {
        "id": "B317GADkSRz5",
        "outputId": "c20ae625-3a56-44fd-ab29-df04c8926099",
        "colab": {
          "base_uri": "https://localhost:8080/"
        }
      },
      "execution_count": null,
      "outputs": [
        {
          "output_type": "stream",
          "name": "stdout",
          "text": [
            "{'rouge1': AggregateScore(low=Score(precision=0.29268871189474543, recall=0.42151709807189086, fmeasure=0.33100955196548326), mid=Score(precision=0.3168492643375833, recall=0.44403236783014755, fmeasure=0.3496622398232095), high=Score(precision=0.3393204852572727, recall=0.4670580213920641, fmeasure=0.3675713685138049)), 'rouge2': AggregateScore(low=Score(precision=0.0788537086389704, recall=0.11486690888240596, fmeasure=0.08958559473587473), mid=Score(precision=0.0894407578299502, recall=0.13139963295047716, fmeasure=0.10122709697733837), high=Score(precision=0.10022051985893649, recall=0.14769454632541706, fmeasure=0.11328097256721148)), 'rougeL': AggregateScore(low=Score(precision=0.15187087240791686, recall=0.21987397956474466, fmeasure=0.17202997488064392), mid=Score(precision=0.16355885762573924, recall=0.23495558222730772, fmeasure=0.1817314216724077), high=Score(precision=0.17527821268837154, recall=0.2519329124882691, fmeasure=0.19164282724874696)), 'rougeLsum': AggregateScore(low=Score(precision=0.2252139228673583, recall=0.3217918890572772, fmeasure=0.2526110747841835), mid=Score(precision=0.24420552124991043, recall=0.33932389423101283, fmeasure=0.2687514097908654), high=Score(precision=0.2624038932523198, recall=0.3573961234310383, fmeasure=0.2836104649349494))}\n"
          ]
        }
      ]
    },
    {
      "cell_type": "code",
      "source": [
        "#compression_opts = dict(method='zip', archive_name='out.csv')  \n",
        "#output.to_csv('out.zip', index=False, compression=compression_opts)\n",
        "\n",
        "#r'C:\\path\\to\\directory\\filename.csv'\n",
        "#import os  \n",
        "#os.makedirs(r'C:\\Users\\manasiganti\\Downloads\\baseline_output', exist_ok=True)  \n",
        "\n",
        "output.to_csv('out_pubmed_lexrank.csv', index = False)  \n",
        "!cp out_pubmed_lexrank.csv \"drive/My Drive/model output\"\n"
      ],
      "metadata": {
        "id": "Qn3o2sWLRoMt"
      },
      "execution_count": null,
      "outputs": []
    }
  ]
}