On the Synchrotron Self-Compton Emission from Relativistic Shocks and Its Implications for Gamma-Ray Burst Afterglows
On the Synchrotron Self-Compton Emission from Relativistic Shocks and Its Implications for Gamma-Ray Burst Afterglows
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DOI：
10.1086/319003
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发表时间：
2000-05
期刊：
影响因子：
--
通讯作者：
R. Sari;A. Esin
中科院分区：
文献类型：
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作者：
R. Sari;A. Esin
研究了γ射线暴余辉中同步辐射光子与相对论电子的逆康普顿散射效应。我们计算了逆康普顿辐射的光谱，发现它可以在初始爆炸后的几个月甚至几年内主导余辉的总冷却速率。我们表明，存在强逆康普顿冷却可以推断出它的效果上的时间演化的冷却中断的同步辐射光谱组件，因此在光学和X射线余辉光曲线。然后，我们将展示如何的物理解释所观察到的同步加速器光谱的特性必须修改，以考虑到这个额外的冷却源，并给出了一个修改后的处方计算的物理参数，从所观察到的数量的特征扩展冲击波。我们发现，对于一组给定的观测值（同步辐射中断频率和通量），要么没有一致的物理解释，要么有两个。最后讨论了利用Chandra直接探测逆康普顿辐射的前景。我们认为，这样的检测是可能的伽玛暴爆炸在一个合理的密度（n <$1 cm-3）的介质。
We consider the effects of inverse Compton scattering of synchrotron photons from relativistic electrons in γ-ray burst (GRB) afterglows. We compute the spectrum of the inverse Compton emission and find that it can dominate the total cooling rate of the afterglow for several months or even years after the initial explosion. We demonstrate that the presence of strong inverse Compton cooling can be deduced from the effect it has on the time evolution of the cooling break in the synchrotron spectral component, and therefore on the optical and X-ray afterglow light curves. We then show how the physical interpretation of the observed characteristics of the synchrotron spectrum must be modified to take into consideration this extra source of cooling and give a revised prescription for computing physical parameters characterizing the expanding shock wave from the observed quantities. We find that for a given set of observables (synchrotron break frequencies and fluxes) there is either no consistent physical interpretation or two of them. Finally we discuss the prospects of directly detecting the inverse Compton emission with Chandra. We argue that such a detection is possible for GRBs exploding in a reasonably dense (n ≳ 1 cm-3) medium.