Modelling the GeV emission of HESS J0632+057
Modelling the GeV emission of HESS J0632+057
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DOI：
10.1093/mnras/stx1928
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发表时间：
2017-07
影响因子：
4.8
通讯作者：
S. Yi;K. Cheng
中科院分区：
文献类型：
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作者：
S. Yi;K. Cheng
最近，费米发现HESS J 0632 +057双星系统具有轨道调制的GeV辐射。本文研究了HESS J 0632 +057的致密伴星是脉冲星的可能性。在这样的假设下，我们重点研究了该系统的高能发射机制，具体如下。脉冲星的伴星在每个轨道上穿过主序星星星的拱星盘两次，这时一些物质被引力捕获。被捕获的物质在脉冲星周围形成一个吸积盘，来自吸积盘的软光子被脉冲星风逆康普顿散射，成为系统的GeV辐射。选择适当的参数，可以得到与观测值相符合的自相关系数和光变曲线。我们预言GeV辐射的光变曲线有两个峰值，较大的峰值在近星点后0.4附近（或X射线极大值后0.1），较小的峰值在0 - 0.1相位之间，积分通量是较大峰值的四分之一。
The binary system HESS J0632+057 was recently detected by {Fermi} to possess orbital modulated GeV emission. In this paper, we study the possibility that the compact companion of HESS J0632+057 is a pulsar. Under such a presumption, we focus on the high energy emission mechanism of this system, which is as follows. The pulsar companion travels through the circumstellar disc of the main sequence star twice in each orbit, when some of the matter is gravity-captured. The captured matter develops an accretion disc around the pulsar, and the soft photons from which are inverse Compton scattered by the pulsar wind as the GeV emission from the system. With proper choice of parameters, SED and light curve which are in accordance with observations can be produced. We predict that the light curve of GeV emission has two peaks, the larger one is at around 0.4 after the periastron (or 0.1 after the X-ray maximum), while the smaller one is between phases 0 and 0.1, with integrated flux one forth of the larger one.