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RIMOTSによるGRB041006の可視光残光の早期観測
http://hdl.handle.net/10458/359
http://hdl.handle.net/10458/359b8e9351a-0372-4390-a793-8a511d2e5a9b
| 名前 / ファイル | ライセンス | アクション |
|---|---|---|
KJ00003579350.pdf (977.3 kB)
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| Item type | 紀要論文 / Departmental Bulletin Paper(1) | |||||||||||
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| 公開日 | 2007-06-28 | |||||||||||
| タイトル | ||||||||||||
| タイトル | RIMOTSによるGRB041006の可視光残光の早期観測 | |||||||||||
| 言語 | ja | |||||||||||
| タイトル | ||||||||||||
| タイトル | The Earliest Optical Afterglow of GRB041006 Observed By RIMOTS | |||||||||||
| 言語 | en | |||||||||||
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| 言語 | jpn | |||||||||||
| キーワード | ||||||||||||
| 言語 | en | |||||||||||
| 主題Scheme | Other | |||||||||||
| 主題 | Astrophysics, Gamma-Ray Burst, GRB041006, Optical Observation, Afterglow, Synchrotron shock | |||||||||||
| 資源タイプ | ||||||||||||
| 資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||||||||
| 資源タイプ | departmental bulletin paper | |||||||||||
| その他（別言語等）のタイトル | ||||||||||||
| その他のタイトル | RIMOTS ニ ヨル GRB041006 ノ カシコウ ザンコウ ノ ソウキ カンソク | |||||||||||
| 言語 | ja-Kana | |||||||||||
| 著者 |
園田, 絵里
× 園田, 絵里× 山内, 誠
WEKO
11882
× 前野, 将太× 山本, 幹生× 松尾, 嘉比古× 河合, 誠之× 小浜, 光洋× 園田, 絵里× 前野, 将太× Matsuo, Yoshihiko× 河合, 誠之× 小浜, 光洋 |
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| 抄録 | ||||||||||||
| 内容記述タイプ | Abstract | |||||||||||
| 内容記述 | GRB041006 was first detected by HETE-2 on 2004 Oct. 6 at 12:18:08 UT. We have observed it's earliest optical afterglow from 12:19:18 UT to through the night. Our observation was performed by using the unfiltered CCD camera on the 30-cm telescope. We combined our converted R band data with those reported by GCN. Statistics don't allow us to say in detail but the light curve shows two slope changes. The power-low index α of the flux decay is α =0.62 before about 0.0053 day after the burst, α =-0.45 from 0.0053 day to 0.077 day after the burst, and α =-1 after 0.077 day. These index changes can be explained by forward shock in synchrotron shock model. During the first flat period, optical emission is generated by cooling of all electrons, which are accelerated by forward shock. But the speed of the shell become slower, then the critical frequency becomes lower than the optical band. The light curve, therefore, got dark slowly. And finally, since the minimum frequency at which the slowest ones among the accelerated electrons emit is below the optical frequency, the electrons that can emit optical light decrease rapidly. So the afterglow darkened fast. |
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| 言語 | en | |||||||||||
| 書誌情報 |
ja : 宮崎大学工学部紀要 en : Memoirs of Faculty of Engineering, University of Miyazaki 巻 34, p. 15-21, 発行日 2005-08 |
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| 出版者 | ||||||||||||
| 出版者 | 宮崎大学工学部 | |||||||||||
| 言語 | ja | |||||||||||
| 出版者 | ||||||||||||
| 出版者 | Faculty of Engineering, University of Miyazaki | |||||||||||
| 言語 | en | |||||||||||
| ISSN | ||||||||||||
| 収録物識別子タイプ | ISSN | |||||||||||
| 収録物識別子 | 05404924 | |||||||||||
| 書誌レコードID | ||||||||||||
| 収録物識別子タイプ | NCID | |||||||||||
| 収録物識別子 | AA00732558 | |||||||||||
| 著者版フラグ | ||||||||||||
| 出版タイプ | VoR | |||||||||||
| 出版タイプResource | http://purl.org/coar/version/c_970fb48d4fbd8a85 | |||||||||||
