| 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 |
A spatial and spectral study of nonthermal filaments in historical supernova remnants: Observational results with Chandra |
|
言語 |
en |
| 作成者 |
Bamba, Aya
Yamazaki, Ryo
Yoshida, Tatsuo
Terasawa, Toshio
Koyama, Katsuji
|
| 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 ISM |
| 主題 |
|
|
主題Scheme |
Other |
|
主題 |
individual(Cassiopeia A, Kepler's Supernova Remnant G120.1+1.4, SN 1006, RCW 86) |
| 主題 |
|
|
主題Scheme |
Other |
|
主題 |
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 outer shells of young supernova remnants (SNRs) are the most plausible acceleration sites of high-energy electrons with the diffusive shock acceleration (DSA) mechanism. We studied spatial and spectral properties close to the shock fronts in four historical SNRs (Cas A, Kepler's remnant, Tycho's remnant, and RCW86) with excellent spatial resolution of Chandra. In all of the SNRs, hard X-ray emissions were found on the rims of the SNRs, which concentrate in very narrow regions ( so-called filaments); apparent scale widths on the upstreamside are below or on the order of the point-spread function of Chandra, while they are 0.'' 5 - 40 '' (0.01 - 0.4 pc) on the downstream side with most reliable distances. The spectra of these filaments can be fitted with both thermal and nonthermal ( power law and SRCUT) models. The former requires unrealistic high temperature (greater than or similar to 2 keV) and low abundances (less than or similar to 1 solar) for emission from young SNRs and may be thus unlikely. The latter reproduces the spectra with best-fit photon indices of 2.1 - 3.8, or roll-off frequencies of (0.1 28) x 10(17) Hz, which reminds us of the synchrotron emission from electrons accelerated via DSA. We consider various physical parameters as functions of the SNR age, including the previous results on SN 1006; the filament width on the downstream side increases with the SNR age, and the spectrum becomes softer, keeping a nonthermal feature. It was also found that a function, that is, the roll-off frequency divided by the square of the scale width on the downstream side, shows negative correlation with the age, which might provide us some information on the DSA theory. |
|
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 |
10.1086/427620 |
| 関連情報 |
|
|
|
識別子タイプ |
DOI |
|
|
関連識別子 |
http://dx.doi.org/10.1086/427620 |
| 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 |
793 |
| 書誌情報 |
Astrophysical Journal
Astrophysical Journal
巻 621,
号 2,
p. 793-802,
発行日 2005-03
|
| 旧ID |
14645 |
AstrophysJ_621_793.pdf (653.0 KB)
