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The Structure of the Pulsar Magnetosphere via Particle Simulation
https://jaxa.repo.nii.ac.jp/records/5017
https://jaxa.repo.nii.ac.jp/records/501783530e9d-341f-45fe-96db-b48c073c06c0
名前 / ファイル | ライセンス | アクション |
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64574085.pdf (186.2 kB)
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Item type | 会議発表論文 / Conference Paper(1) | |||||
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公開日 | 2015-03-26 | |||||
タイトル | ||||||
言語 | en | |||||
タイトル | The Structure of the Pulsar Magnetosphere via Particle Simulation | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | pulsars: general - magnetic field - plasmas | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_5794 | |||||
資源タイプ | conference paper | |||||
著者 |
柴田, 晋平
× 柴田, 晋平× 結城, 伸哉× 和田, 智秀× 海崎, 光宏× Shibata, Shinpei× Yuki, Shinya× Wada, Tomohide× Umizaki, Mitsuhiro |
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著者所属 | ||||||
山形大学理学部 | ||||||
著者所属 | ||||||
山形大学大学院理工学研究科 | ||||||
著者所属 | ||||||
国立天文台天文学データ解析計算センター | ||||||
著者所属 | ||||||
山形大学大学院理工学研究科 | ||||||
著者所属(英) | ||||||
en | ||||||
Department of Physics, Yamagata University | ||||||
著者所属(英) | ||||||
en | ||||||
Graduate School of Science and Engineering, Yamagata University | ||||||
著者所属(英) | ||||||
en | ||||||
Center for Computational Astrophysics, National Astronomical Observatory of Japan | ||||||
著者所属(英) | ||||||
en | ||||||
Graduate School of Science and Engineering, Yamagata University | ||||||
出版者 | ||||||
出版者 | 宇宙航空研究開発機構 | |||||
出版者(英) | ||||||
出版者 | Japan Aerospace Exploration Agency (JAXA) | |||||
書誌情報 |
宇宙航空研究開発機構特別資料: en : JAXA Special Publication: The Energetic Cosmos; from Suzaku to ASTRO-H 巻 JAXA-SP-09-008E, p. 226-227, 発行日 2010-02-26 |
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会議概要(会議名, 開催地, 会期, 主催者等)(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan | |||||
抄録(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | 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. | |||||
内容記述(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science | |||||
ISSN | ||||||
収録物識別子タイプ | ISSN | |||||
収録物識別子 | 1349-113X | |||||
書誌レコードID | ||||||
収録物識別子タイプ | NCID | |||||
収録物識別子 | AA11984031 | |||||
資料番号 | ||||||
内容記述タイプ | Other | |||||
内容記述 | 資料番号: AA0064574085 | |||||
レポート番号 | ||||||
内容記述タイプ | Other | |||||
内容記述 | レポート番号: JAXA-SP-09-008E |