伽马射线暴中快升慢衰子脉冲的模型
A Model for Fast Rising, Slowly Decaying Subpulses in Gamma-Ray Bursts
摘要：
伽马射线暴（GRB）的特征通常是具有明显不对称轮廓的子脉冲--它们上升得很快，衰减得慢得多，而它们的光谱随着观察者的时间而稍微软化。有人认为，这些次脉冲是由嵌在初级$γ$射线束中的慢重子云引起的，当它们加速时，这些慢重子云将$γ$辐射散射到我们的视线中。与观测到的光变曲线和光谱演化得到了很好的定量一致性。伽玛射线暴喷流的重子成分从初级$γ$辐射中获得的动能预计大约等于散射的$γ$辐射量，这与余辉观测结果一致。其他几个观测结果进行了简要讨论。提出了短伽玛暴的时间尺度是由辐射加速和/或重子注入而不是由中央引擎的时间尺度建立的可能性。
英文摘要：
Gamma ray bursts (GRB's) often feature subpulses that have a distinctively asymmetric profile -- they rise quickly and decay much more slowly, while their spectrum softens slightly with observer time. It is suggested that these subpulses are caused by slow baryonic clouds embedded within a primary $γ$-ray beam, which scatter the $γ$-radiation into our line of sight as they accelerate. Good quantitative agreement is obtained with observed light curves and spectral evolution. The kinetic energy that the baryonic component of GRB jets receives from the primary $γ$-radiation is predicted to be about equal to the amount of $γ$-radiation that is scattered, consistent with observations of afterglow. Several other observational consequences are briefly discussed. The possibility is raised that the time scale of short GRB is established by radiative acceleration and/or baryon injection rather than the time scale of the central engine.
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