Inverse Compton emission from a cosmic-ray precursor in RX J1713.7-3946
Inverse Compton emission from a cosmic-ray precursor in RX J1713.7-3946
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DOI：
10.1016/j.jheap.2017.03.001
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发表时间：
2017-03-01
影响因子：
3.8
通讯作者：
Yamazaki, Ryo
中科院分区：
文献类型：
--
作者：
Ohira, Yutaka;Yamazaki, Ryo
最近，高能立体系统（HESS）报告了两个关于伽马射线发射超新星遗迹RX J1713.7-3946（G347.3-0.5）的新的有趣结果。第一个结果是建立了GeV-TeV伽马射线的破幂律谱。另一个是一个更广泛的伽马射线空间分布比一个在X射线波段。在本文中，我们表明，这两个结果可以解释从加速电子的逆康普顿发射。如果被加速的电子的最大能量随时间减小，则可以通过累积产生破幂律谱。此外，γ射线分布的扩展分量可以解释为当前加速电子的CR前驱体。(C)2017爱思唯尔B. V.保留所有权利。
Recently, the High Energy Stereoscopic System (H.E.S.S.) reported two new interesting results for a gamma-ray emitting supernova remnant, RX J1713.7-3946 (G347.3-0.5). The first result is the establishment of a broken power-law spectrum of GeV-TeV gamma-rays. The other is a more extended gamma-ray spatial profile than the one in the X-ray band. In this paper, we show both of these results can be explained by inverse Compton emission from accelerated electrons. If the maximum energy of electrons being accelerated decreases with time, the broken power-law spectrum can be generated by accumulation. Furthermore, the extended component of gamma-ray profile can be interpreted as a CR precursor of currently accelerated electrons. (C) 2017 Elsevier B.V. All rights reserved.