@inproceedings{oai:jaxa.repo.nii.ac.jp:00005017,
 author = {柴田, 晋平 and 結城, 伸哉 and 和田, 智秀 and 海崎, 光宏 and Shibata, Shinpei and Yuki, Shinya and Wada, Tomohide and Umizaki, Mitsuhiro},
 book = {宇宙航空研究開発機構特別資料:, JAXA Special Publication: The Energetic Cosmos; from Suzaku to ASTRO-H},
 month = {Feb},
 note = {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},
 pages = {226--227},
 publisher = {宇宙航空研究開発機構, Japan Aerospace Exploration Agency (JAXA)},
 title = {The Structure of the Pulsar Magnetosphere via Particle Simulation},
 volume = {JAXA-SP-09-008E},
 year = {2010}
}