| Project/Area Number |
10640234
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
Astronomy
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| Research Institution | RIKKYO UNIVERSITY |
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Principal Investigator |
SHIBAZAKI Noriaki (1999-2000) RIKKYO UNIV., COLLEGE OF SCIENCE, PROFESSOR, 理学部, 教授 (50206124)
蓬茨 霊運 (1998) 立教大学, 理学部, 教授 (70062601)
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| Co-Investigator(Kenkyū-buntansha) |
柴崎 徳明 立教大学, 理学部, 教授 (50206124)
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| Project Period (FY) |
1998 – 2000
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| Project Status |
Completed (Fiscal Year 2000)
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| Budget Amount *help |
¥2,500,000 (Direct Cost: ¥2,500,000)
Fiscal Year 2000: ¥700,000 (Direct Cost: ¥700,000)
Fiscal Year 1999: ¥600,000 (Direct Cost: ¥600,000)
Fiscal Year 1998: ¥1,200,000 (Direct Cost: ¥1,200,000)
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| Keywords | accretion disk / blackhole / X &γ ray emission / astrophysical jet / SS 433 / ガンマ線バースト / 残光現象 / ジェット加速 / X線連星 / X線新星 / 中性子星 |
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| Research Abstract |
Black holes in the binary systems and active galactic nuclei are surrounded with an accretion disk. Astrophysical jets, observed in SS 433 and brazers, are considered to be ejected from the accretion disk. Recently, X-ray observations are yielding an important progress on the SS 433 jets. Hence, we focused on the SS 433 jets and studied the structure and emission of the SS 433 jets. The main results of this study are summarized as follows.
(1) We can derive the analytical solutions that determine the temperature distribution along the jet. In the inner part of a jet the ion and electron temepratures are different and the jet is optically thick, whereas in the outer part two temperatures are the same and the jet is optically thin.
(2) The jet is conical near the central object, while in the outer part the jet cross section increases with distance from the central object.
(3) The sonic point is located at the distance of〜9×10^7 cm, which excludes the gas pressure as a possible mechanism for jet acceleration.
(4) The radiation pressure is also ruled out as a possible acceleration mechanism since the inner part of the jet is optically thick.
(5) The jet solution we found predicts a gamma ray emission, which amounts to〜10^<39> erg/s. No observation of such gamma rays indicates that the inner part of the jet is screened by a thick accretion disk.
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