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Numerical Study of Propagation of UHECRs: Spectrum, Arrival Direction, Composition

机译：UHECRs传播的数值研究：频谱，到达方向，组成

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摘要

In this paper, simulations of propagation of UHE-protons from nearby galaxies are presented. We found goodparameter sets to explain the arrival distribution of UHECRs reported by AGASA and the energy spectrum reported byHiRes. Using a good parameter set, we demonstrated what distribution of arrival direction of UHECRs will be as afunction of event numbers. We show that 1000-10000 events are necessary to clearly see the source distribution. We alsoshowed that effects of interactions and trapping of UHE-Nuclei in a galaxy cluster are very important. Especially, whena UHECR source is a bursting source such as a GRB/AGN flare, heavy UHE-Nuclei are trapped for a long time in thegalaxy cluster, which changes the spectrum and chemical composition of UHECRs coming from the galaxy cluster. Wealso showed that such effects can be important when there have been sources of UHE-Nuclei in the Milky Way. Sincelight nuclei escape from the Milky Way in a short timescale, the chemical composition of UHECRs observed at the Earthcan be heavy at the high-energy range as suggested by Auger.
机译：在本文中，模拟了UHE质子从附近星系的传播。我们找到了很好的参数集来解释AGASA报告的UHECR的到达分布和HiRes报告的能谱。使用一个好的参数集，我们证明了UHECR到达方向的分布将是事件编号的函数。我们表明，必须有1000-10000个事件才能清楚地看到源分布。我们还表明，星系团中UHE-核子的相互作用和俘获作用非常重要。特别是当UHECR源是诸如GRB / AGN耀斑之类的爆发源时，重的UHE-核子会长时间滞留在星系团中，这会改变来自星系团的UHECR的光谱和化学成分。我们还表明，当银河系中存在UHE-Nuclei来源时，此类影响可能很重要。由于轻核在很短的时间内从银河系中逃逸，因此，如俄格（Auger）建议的那样，在地球上观察到的UHECR的化学成分在高能范围内可能很重。

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  • 会议地点 Beijing(CN)
  • 作者

    S.NAGATAKI; T.PIEROG; A.R.VAN VLIET; O.SCHOLTEN; H.YOSHIGUCHI; K.SATO; D.ALLARD; K.KOTERA; A.CALVEZ; A.KUSENKO; K.MURASE; J.AOI; Y.DUBOIS;

  • 作者单位

    Yukawa Institute for Theoretical Physics Kyoto University Oiwake-cho Kitashirakawa Sakyo-ku Kyoto 606-8502 Japan;

    Forschungszentrum Karlsruhe Institut fuer Kernphysik Karlsruhe Germany;

    Kernfysisch Versneller Instituut University of Groningen 9747 AA Groningen The Netherlands;

    Department of Physics School of Science the University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo 113-0033 Japan;

    National Institutes of Natural Sciences 4-3-13 Toranomon Minato-ku Tokyo 105-0001 Japan The Institute for the Physics and Mathematics of the Universe The University of Tokyo 5-1-5 Kashiwanoha Kashiwa Chiba 277-8568 Japan Department of Physics School of Science and Engineering Meisei University 2-1-1 Hodokubo Hino Tokyo 191-8506 Japan;

    Laboratoire Astroparticules et Cosmologie Universite Paris 7/CNRS 10 Rue A. Domon et L. Duquet 75205 Paris Cedex 13 France;

    Department of Astronomy & Astrophysics Enrico Fermi Institute and Kavli Institute for Cosmological Physics The University of Chicago 5640 S. Ellis Ave Chicago IL 60637 USA;

    Department of Physics and Astronomy University of California Los Angeles California 90095-1547 USA;

    The Institute for the Physics and Mathematics of the Universe The University of Tokyo 5-1-5 Kashiwanoha Kashiwa Chiba 277-8568 Japan Department of Physics and Astronomy University of California Los Angeles California 90095-1547 USA;

    CCAPP OSU 191 W. Woodruff Ave. Columbus Ohio 43210 USA;

    University of Oxford Astrophysics Denys Wilkinson Building Keble Road Oxford OX1 3RH UK;

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  • 关键词

    UHECRs; Spectrum; Arrival Direction; Composition;

    机译：UHECR；光谱;到达方向；组成;

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