| 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 |
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|
タイトル |
Constraints on the diffusive shock acceleration from the nonthermal X-ray thin shells in SN 1006 NE rim |
|
言語 |
en |
| 作成者 |
Yamazaki, Ryo
Yoshida, T.
Terasawa, T.
Banba, A.
Koyama, K.
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| アクセス権 |
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|
アクセス権 |
open access |
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アクセス権URI |
http://purl.org/coar/access_right/c_abf2 |
| 権利情報 |
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権利情報 |
Copyright (c) 2004 ESO |
| 主題 |
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|
主題Scheme |
Other |
|
主題 |
acceleration of particles - ISM |
| 主題 |
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主題Scheme |
Other |
|
主題 |
supernova remnants - X-rays |
| 主題 |
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主題Scheme |
Other |
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主題 |
ndividual |
| 主題 |
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|
主題Scheme |
Other |
|
主題 |
SN 1006 |
| 主題 |
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|
主題Scheme |
NDC |
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主題 |
440 |
| 内容記述 |
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内容記述 |
Characteristic scale lengths of nonthermal X-rays from the SN 1006 NE rim, which are observed by Chandra, are interpreted in the context of diffusive shock acceleration with the assumption that the observed spatial profile of nonthermal X-rays corresponds to that of accelerated electrons with energies of a few tens of TeV. To explain the observed scale lengths, we construct two simple models with a test particle approximation, where the maximum energy of accelerated electrons is determined by the age of SN 1006 (age-limited model) or the energy loss (energy loss-limited model), and constrain the magnetic field configuration and the diffusion coefficients of accelerated electrons. When the magnetic field is nearly parallel to the shock normal, the magnetic field should be in the range of 20-85 uG and highly turbulent both upstream and downstream, which means that the mean free path of accelerated electrons is of the order of their gyro-radius (Bohm limit). This situation can be realized both in the age-limited and energy loss-limited model. On the other hand, when the magnetic field is nearly perpendicular to the shock normal, which can exist only in the age-limited case, the magnetic field is several uG upstream and 14-20 uG downstream, and the upstream magnetic field is less turbulent than the downstream. |
|
言語 |
en |
| 出版者 |
|
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出版者 |
EDP Science |
| 言語 |
|
|
言語 |
eng |
| 資源タイプ |
|
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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 |
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識別子タイプ |
DOI |
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関連識別子 |
10.1051/0004-6361:20034212 |
| 関連情報 |
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|
関連タイプ |
isVersionOf |
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|
識別子タイプ |
DOI |
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|
関連識別子 |
http://dx.doi.org/10.1051/0004-6361:20034212 |
| 収録物識別子 |
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収録物識別子タイプ |
ISSN |
|
収録物識別子 |
0004-6361 |
| 開始ページ |
|
|
開始ページ |
595 |
| 書誌情報 |
Astronomy Astrophysics
Astronomy Astrophysics
巻 416,
号 2,
p. 595-602,
発行日 2004
|
| 旧ID |
14773 |
AA_416_2_595.pdf (205.1 KB)
