2018 Fiscal Year Final Research Report
Study of very high energy gamma-ray emission region and emission mechanism in non-blazar active galactic nuclei
| Project/Area Number |
16K05381
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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| Allocation Type | Multi-year Fund |
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| Section | 一般 |
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| Research Field |
Particle/Nuclear/Cosmic ray/Astro physics
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| Research Institution | Tokai University |
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Principal Investigator |
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| Co-Investigator(Kenkyū-buntansha) |
櫛田 淳子 東海大学, 理学部, 教授 (80366020)
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| Research Collaborator |
KINO Motoki
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| Project Period (FY) |
2016-04-01 – 2019-03-31
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| Keywords | 宇宙線 / 活動銀河核 / 超エネルギーガンマ線 / 電波銀河 / 超大質量ブラックホール / 相対論的ジェット / M87 / マルチメッセンジャー |
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| Outline of Final Research Achievements |
It is generally accepted that there are super-massive black holes in the center of active galactic nuclei(AGNs) and extremely violent astrophysical phenomena occur around there. Blazars, whose relativistic jets point toward us, are known to be one of the very high energy gamma-ray sources. However, recently, very high energy gamma rays from non-blazar AGNs are observed unexpectedly, and the emission mechanism is still a mystery. So we aim to localize the emission region of very high energy gamma rays in radio galaxies and to study the emission mechanisms by observing radio galaxy M 87 with the Imaging atmospheric Cherenkov Telescope, MAGIC. Then, we successfully observed very high energy gamma rays from M 87, and we constrained the size of the emission region got a clue of the emission mechanism.
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| Free Research Field |
宇宙線物理学
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| Academic Significance and Societal Importance of the Research Achievements |
本研究は，超大質量ブラックホール周辺の極限状態における天体物理現象の解明に，超高エネルギーガンマ線の観測から迫ろうとするものである．その内容は，宇宙線物理学としての宇宙線の起源，プラズマ物理学としての荷電粒子と磁場の相互作用による加速機構，素粒子物理学としての粒子相互作用の素過程，高エネルギー宇宙物理学としての天体物理現象の解明．天文学としての銀河の共進化，宇宙論としての宇宙の進化等，極めて幅広い分野の基礎的研究に関係する成果であり，人類の知見を広めることに少なからず貢献している．
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