Quasi-thermal Comptonization and Gamma-Ray Bursts
Quasi-thermal Comptonization and Gamma-Ray Bursts
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DOI：
10.1086/311845
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发表时间：
1998-12
期刊：
影响因子：
--
通讯作者：
G. Ghisellini;A. Celotti
中科院分区：
文献类型：
--
作者：
G. Ghisellini;A. Celotti
在相对论壳层之间形成的内部激波中的准热康普顿化可以解释伽马射线暴的高能发射。如果发射粒子的典型能量是通过加热和冷却之间的平衡或作为电子-正电子对产生的结果来实现的，则这实际上是主要的冷却机制。这两个过程都产生次相对论性或轻度相对论性能量。在这种情况下，同步辐射光谱是自吸收的，为康普顿化过程提供了软种子光子，其光谱是平坦的[F（v）~const]，根据发射粒子的散射光学深度，以指数截止或维恩峰结束。自洽粒子的能量和光学深度的估计，发现与观察到的光谱。
Quasi-thermal Comptonization in internal shocks formed between relativistic shells can account for the high-energy emission of gamma-ray bursts. This is in fact the dominant cooling mechanism if the typical energy of the emitting particles is achieved either through the balance between heating and cooling or as a result of electron-positron pair production. Both processes yield subrelativistic or mildly relativistic energies. In this case, the synchrotron spectrum is self-absorbed, providing the soft-seed photons for the Comptonization process, whose spectrum is flat [F(ν)~const], ending in either an exponential cutoff or a Wien peak, depending on the scattering optical depth of the emitting particles. The self-consistent particle energy and optical depth are estimated and found in agreement with the observed spectra.