| Co-Investigator(Kenkyū-buntansha) |
HOSHINO Masahiro The University of Tokyo, Department of Earth and Planetary Science, Professor, 大学院・理学系研究科, 教授 (90241257)
YOKOYAMA Takaaki The University of Tokyo, Department of Earth and Planetary Science, Associate Professor, 大学院・理学系研究科, 助教授 (00311184)
TAKAHARA Fumio University of Oosaka, Department of Earth and Space Science, Professor, 大学院・理学研究科, 教授 (20154891)
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| Budget Amount *help |
¥13,700,000 (Direct Cost: ¥13,700,000)
Fiscal Year 2004: ¥3,300,000 (Direct Cost: ¥3,300,000)
Fiscal Year 2003: ¥3,400,000 (Direct Cost: ¥3,400,000)
Fiscal Year 2002: ¥7,000,000 (Direct Cost: ¥7,000,000)
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| Research Abstract |
Shock particle accelerations are taking place in various environments, such as solar flares, interplanetary shocks formed in front of coronal mass ejecta (CME), the bow shock in front of the earth, shocks associating with corotating interaction regions, the solar wind terminating shock, shocks in the supernova blast waves, pulsar wind terminating shocks, terminating shocks at the AGN jets, inner and external shocks in gamma ray bursters, cosmological shocks relating to the structual formation, and slow shocks relatng to the magnetic re connection process. While in both fields, solar wind plasma physics and astrophysical plasma physics, the research activities in Japan are competing well in the world, we are conducting a collaborating research project by which we could envisage the further research development. Fortunately our three-year project has been quite successful. In what follows, we itemize the significant accomplishments in five areas, namely, 1.elementary shock process, 2.rel
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ativistic plasmas/jets and GRBs, 3.solar corona and flares, 4.the earth's bow shock, interplanetary field, and heliosphere, and 5.magnetosphere.
Category 1 : mathematical theory of stochastic process has been successfully applied to the shock acceleration process. The idea of the surfin acceleration is developed further.
Category2 : The GRB cascade model and wien fireball model are formulated. Acceleration efficiency in AGN shocks are identified. Successful defections of gamma ray photons from the giant burst of SGR1806-20.
Category 3 : Successful observation of subrelativistic electron propagation in the corona. The role of nonlinear waves and helicities in the corona are identified. The low energy cutoff of the X-ray spectra of solar flares are identified.
Category 4 : For the fastest interplanetary shocks ever recorded, shock parameters are deterined successfully. Acceleration processes for interstellar He+ ions and foreshock diffuse ions are identified.
Category 5 : The structure of the magnetotail current sheet is identified.
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