Detection of the hard X-ray non-thermal emission from Kepler’s supernova remnant
Detection of the hard X-ray non-thermal emission from Kepler’s supernova remnant
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开普勒超新星遗迹的硬 X 射线非热辐射探测
DOI：
10.1093/pasj/psaa121
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发表时间：
2021
影响因子：
2.3
通讯作者：
Terada Yukikatsu
中科院分区：
文献类型：
--
作者：
Nagayoshi Tsutomu;Bamba Aya;Katsuda Satoru;Terada Yukikatsu
我们报告的硬X射线探测器（HXD-PIN）的硅PIN型半导体探测器的朱雀星上的硬X射线探测器的第一个强大的探测器在15-30 keV波段从开普勒的超新星遗迹的硬X射线发射。对于开普勒整个X射线发射区的发射，探测显著性为7.17σ。的能谱被发现是很好地再现由一个单一的幂律函数与光子指数，其中的第一和第二个错误代表统计和系统误差，分别。X射线通量在15-30 keV波段被确定为s−1cm− 2。结合软X射线Suzaku/XIS光谱的3-30 keV波段的更宽波段X射线光谱表明，非热成分不具有显着的X射线滚降结构。我们发现，在滚降能量为1.0 × 10 ~（17）Hz，磁场强度B> 40 μG的单带轻子模型下，可以再现射电波段、X射线数据和TeV上限的宽带能谱。使用软X射线和硬X射线波段中的指数对数据进行诊断的方法的应用表明，开普勒SNR中加速电子的最大能量受到残骸年龄的限制。这与单带轻子模型的结果是一致的。
We report the first robust detection of the hard X-ray emission in the 15–30 keV band from Kepler’s supernova remnant with the silicon PIN-type semiconductor detector of the hard X-ray detector (HXD-PIN) onboard Suzaku. The detection significance is 7.17σ for the emission from Kepler’s entire X-ray emitting region. The energy spectrum is found to be well reproduced by a single power-law function with a photon index of, where the first and second errors represent-statistical and systematic errors, respectively. The X-ray flux is determined to beerg s−1cm−2in the 15–30 keV band. The wider-band X-ray spectrum in the 3–30 keV band, where the soft X-ray Suzaku/XIS spectrum is combined, shows that the non-thermal component does not have a significant X-ray roll-off structure. We find that the broad-band energy spectrum from the radio band, X-ray data of this work, and TeV upper limits can be reproduced with the one-zone leptonic model with a roll-off energy of νroll= 1.0 × 1017Hz and magnetic field strength ofB> 40 μG. Application of the diagnostic method using indices in the soft and hard X-ray band to the data indicates that the maximum energy of the accelerated electrons in Kepler’s SNR is limited by the age of the remnant. The indication is consistent with the results of the one-zone leptonic modeling.
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影响因子：
2.3
作者：
M. Kokubun;K. Makishima;T. Takahashi;T. Murakami;M. Tashiro;Y. Fukazawa;T. Kamae;G. Madejski
通讯作者：
M. Kokubun;K. Makishima;T. Takahashi;T. Murakami;M. Tashiro;Y. Fukazawa;T. Kamae;G. Madejski
影响因子：
2.3
作者：
K. Mitsuda;M. Bautz;Hajime Inoue;Rich Kelley;K. Koyama;H. Kunieda;K. Makishima;Y. Ogawara;
通讯作者：
K. Mitsuda;M. Bautz;Hajime Inoue;Rich Kelley;K. Koyama;H. Kunieda;K. Makishima;Y. Ogawara;
影响因子：
6.5
作者：
R. Krivonos;M. Revnivtsev;A. Lutovinov;S. Sazonov;E. Churazov;R. M. Iki;Moscow;R. Mpa;
通讯作者：
R. Krivonos;M. Revnivtsev;A. Lutovinov;S. Sazonov;E. Churazov;R. M. Iki;Moscow;R. Mpa;
影响因子：
4.8
作者：
M. L. Ahnen;S. Ansoldi;L. A. Antonelli;C. Arcaro;A. Babi'c;B. Banerjee;P. Bangale;U. D. Almeida
通讯作者：
M. L. Ahnen;S. Ansoldi;L. A. Antonelli;C. Arcaro;A. Babi'c;B. Banerjee;P. Bangale;U. D. Almeida
DOI：
--
发表时间：
2002
期刊：
--
影响因子：
--
作者：
E.G.Berezhko;L.T.Ksenofontov;H. I. O. C. Research;Aeronomy;M. Kernphysik
通讯作者：
M. Kernphysik