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Chandra observations of galactic supernova remnant Vela Jr. : A new sample of thin filaments emitting synchrotron X-rays
https://hiroshima.repo.nii.ac.jp/records/2006334
https://hiroshima.repo.nii.ac.jp/records/2006334d5f47677-86d0-4c08-976e-13b0bf78bb08
| 名前 / ファイル | ライセンス | アクション |
|---|---|---|
AstrophysJ_632_294.pdf (361.0 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 | Chandra observations of galactic supernova remnant Vela Jr. : A new sample of thin filaments emitting synchrotron X-rays | |||||||||||
| 言語 | en | |||||||||||
| 作成者 |
Bamba, Aya
× Bamba, Aya
× Yamazaki, Ryo
× Hiraga, Junko S.
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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 | acceleration of particles | |||||||||||
| 主題 | ||||||||||||
| 主題Scheme | Other | |||||||||||
| 主題 | individual (G266.6-1.2, RX J0852.0-4622) supernova remnants | |||||||||||
| 主題 | ||||||||||||
| 主題Scheme | Other | |||||||||||
| 主題 | X-rays | |||||||||||
| 主題 | ||||||||||||
| 主題Scheme | Other | |||||||||||
| 主題 | ISM | |||||||||||
| 主題 | ||||||||||||
| 主題Scheme | NDC | |||||||||||
| 主題 | 440 | |||||||||||
| 内容記述 | ||||||||||||
| 内容記述 | The Galactic supernova remnant (SNR) Vela Jr. (RX J0852.0-4622, G266.6-1.2) shows sharp filamentary structures on its northwestern edge in the hard X-ray band. The filaments are very smooth and located on the extreme outside edge of the remnant. We measured the averaged scale width of the filaments (w(u) and w(d)) with excellent spatial resolution with Chandra, and they are on the order of the size of the point-spread function of Chandra on the upstream side and 49."5 (36."0 - 88."8) on the downstream side. The spectra of the filaments are very hard and have no linelike structure; they were well reproduced with an absorbed power-law model with Gamma = 2.67 (2.55-2.77) or a SRCUT model with v(roll) = 4.3 (3.4-5.3) x 10(16) Hz under the assumption of p = 0.3. These results imply that the hard X-rays are synchrotron radiation emitted by accelerated electrons, as mentioned previously. Using a correlation between the function B equivalent to v(roll)/w(d)(2) d and the SNR age, we estimated the distance and the age of Vela Jr.: the estimated distance and age are 0.33 (0.26-0.50) kpc and 660 (420-1400) yr, respectively. These results are consistent with previous reports, implying that the B-age relation may be a useful tool for estimating the distance and the age of synchrotron X-ray-emitting SNRs. | |||||||||||
| 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 | 10.1086/432711 | |||||||||||
| 関連情報 | ||||||||||||
| 識別子タイプ | DOI | |||||||||||
| 関連識別子 | http://dx.doi.org/10.1086/432711 | |||||||||||
| 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 | 294 | |||||||||||
| 書誌情報 |
Astrophysical Journal Astrophysical Journal 巻 632, 号 1, p. 294-301, 発行日 2005-10 |
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| 旧ID | 14648 | |||||||||||
