SYNCHROTRON SELF-COMPTON EMISSION AS THE ORIGIN OF THE GAMMA-RAY AFTERGLOW OBSERVED IN GRB 980923
SYNCHROTRON SELF-COMPTON EMISSION AS THE ORIGIN OF THE GAMMA-RAY AFTERGLOW OBSERVED IN GRB 980923
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DOI：
10.1088/0004-637x/751/1/33
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发表时间：
2012-01
期刊：
影响因子：
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通讯作者：
N. Fraija;M. González;Willian H. Lee
中科院分区：
文献类型：
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作者：
N. Fraija;M. González;Willian H. Lee
GRB 980923是爆发和瞬态源实验观测到的最明亮的爆发之一。以前的研究已经检测到两个不同的组件，除了主要的提示情节，这是很好地描述了乐队功能。其中第一个是持续时间为10400 s的尾部，而第二个是持续时间为102 s的高能成分。我们总结了观测结果，并提出了一个统一的模型，其中尾部可以被理解为来自前向冲击同步辐射的早期γ射线余辉，而高能量分量来自反向冲击的同步自康普顿。厚壳发射的主要假设之间的一致性和协议的观测值和计算值之间的通量，断裂能量，开始时间，和光谱指数导致的要求，喷出物必须高度磁化。
GRB 980923 was one of the brightest bursts observed by the Burst and Transient Source Experiment. Previous studies have detected two distinct components in addition to the main prompt episode, which is well described by a Band function. The first of these is a tail with a duration of ≃ 400 s, while the second is a high-energy component lasting ≃ 2 s. We summarize the observations and argue for a unified model in which the tail can be understood as the early γ-ray afterglow from forward shock synchrotron emission, while the high-energy component arises from synchrotron self-Compton from the reverse shock. Consistency between the main assumption of thick shell emission and agreement between the observed and computed values for fluxes, break energies, starting times, and spectral indices leads to a requirement that the ejecta must be highly magnetized.