The Structure of the Pulsar Magnetosphere via Particle Simulation

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The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan

We perform a particle simulation to explain the pulsar phenomena from the first principles. It is shown that the outer gaps indeed appear around the null surface. The origin can be understood simply by strong charge separation by emf of the star in tenuous plasma atmosphere. The gap persists under copious paircreation, providing the particle source of the pulsar wind as well as the gamma-ray pulses. If pair creation rate is high, then some magnetic flux is opened and pairs flow out along the opened magnetic flux, i.e., the pulsar wind is formed. At the present capability of computer, the equatorial current sheet with closed magnetic flux is till thick. If pair creation rate is low, then the wind is moderate, and strong radiation drag causes a large scale circular flow in the magnetosphere. The side-wall of the polar cap flow is verified, but locates nearer to the polar axis than expected, i.e., the middle latitude dead zone, which is different from the dead zone of the closed magnetic field lines is found.

Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science

資料番号: AA0064574085

レポート番号: JAXA-SP-09-008E

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詳細情報 詳細情報について

  • CRID
    1050292561262599680
  • NII論文ID
    120006828487
  • NII書誌ID
    AA11984031
  • ISSN
    1349113X
  • Web Site
    http://id.nii.ac.jp/1696/00005011/
  • 本文言語コード
    en
  • 資料種別
    conference paper
  • データソース種別
    • IRDB
    • CiNii Articles

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