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Ep-Eiso correlation in a multiple subjet model of gamma-ray bursts
https://hiroshima.repo.nii.ac.jp/records/2006335
https://hiroshima.repo.nii.ac.jp/records/2006335348d55ea-9ab8-4ce5-869f-a6b48f69f5db
| 名前 / ファイル | ライセンス | アクション |
|---|---|---|
AstrophysJ_635_481.pdf (560.0 KB)
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| Item type | デフォルトアイテムタイプ_（フル）(1) | |||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| 公開日 | 2023-03-18 | |||||||||||
| タイトル | ||||||||||||
| タイトル | Ep-Eiso correlation in a multiple subjet model of gamma-ray bursts | |||||||||||
| 言語 | en | |||||||||||
| 作成者 |
Toma, Kenji
× Toma, Kenji
× Yamazaki, Ryo
× Nakamura, Takashi
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| アクセス権 | ||||||||||||
| アクセス権 | open access | |||||||||||
| アクセス権URI | http://purl.org/coar/access_right/c_abf2 | |||||||||||
| 権利情報 | ||||||||||||
| 権利情報 | Copyright (c) 2005 The American Astronomical Society | |||||||||||
| 主題 | ||||||||||||
| 主題Scheme | Other | |||||||||||
| 主題 | gamma rays | |||||||||||
| 主題 | ||||||||||||
| 主題Scheme | Other | |||||||||||
| 主題 | theory | |||||||||||
| 主題 | ||||||||||||
| 主題Scheme | Other | |||||||||||
| 主題 | bursts | |||||||||||
| 主題 | ||||||||||||
| 主題Scheme | NDC | |||||||||||
| 主題 | 440 | |||||||||||
| 内容記述 | ||||||||||||
| 内容記述 | We perform Monte Carlo simulations to study the Ep-E iso correlation in the context of a multiple-subjet model (or inhomogeneous jet model) for γ-ray bursts (GRBs), X-ray-rich GRBs (XRRs), and X-ray flashes (XRFs). For a single subjet, we find that Ep ∝ Eiso0.4 for large viewing angles. For the multiple-subjet model in which all the subjets have the same intrinsic properties, off-axis events show Ep ∝ Eisoa with 0.4 < a < 0.5. If the intrinsic properties of the subjets are distributed so that on-axis emission of each subjet follows a correlation Ep ∝ Liso1/2, we obtain the Amati correlation (Ep ∝ Eiso1/2) over 3 orders of magnitude in E p. Although the scatter around the Amati correlation is large in the simulation, the results are consistent with the observed properties of GRBs with known redshifts and the BASTE GRBs with pseudoredshifts derived from the lag-luminosity correlation. We also calculate the event rates, the redshift distributions, and the T90 duration distributions of GRBs, XRRs, and XRFs, which can be detected by HETE-2, assuming that the source redshift distribution is in proportion to the cosmic star formation rate. It is found that the event rates of the three classes are comparable, that the average redshift of the XRRs is a little larger than those of the GRBs and the XRFs, and that short XRRs arise when a single subjet is viewed off-axis or viewed on-axis with slightly high redshift. © 2005. The American Astronomical Society. All rights reserved. | |||||||||||
| 言語 | en | |||||||||||
| 出版者 | ||||||||||||
| 出版者 | University of Chicago Press | |||||||||||
| 言語 | ||||||||||||
| 言語 | eng | |||||||||||
| 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 | journal article | |||||||||||
| 出版タイプ | ||||||||||||
| 出版タイプ | VoR | |||||||||||
| 出版タイプResource | http://purl.org/coar/version/c_970fb48d4fbd8a85 | |||||||||||
| 関連情報 | ||||||||||||
| 識別子タイプ | DOI | |||||||||||
| 関連識別子 | 10.1086/497388 | |||||||||||
| 関連情報 | ||||||||||||
| 識別子タイプ | DOI | |||||||||||
| 関連識別子 | http://dx.doi.org/10.1086/497388 | |||||||||||
| 収録物識別子 | ||||||||||||
| 収録物識別子タイプ | ISSN | |||||||||||
| 収録物識別子 | 0004-637X | |||||||||||
| 開始ページ | ||||||||||||
| 開始ページ | 481 | |||||||||||
| 書誌情報 |
Astrophysical Journal Astrophysical Journal 巻 635, 号 1, p. 481-486, 発行日 2005-12 |
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| 旧ID | 14649 | |||||||||||
