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arXiv 0805.0144astro-ph
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我们从伽马射线暴080319 B中学到了什么？

What did we learn from gamma-ray burst 080319B ?

P. Kumar, A. Panaitescu

备注：
5 pages, to appear in MNRAS Letters, potential difficulties of the SSC model discussed in S2.2
发表信息：
Mon.Not.Roy.Astron.Soc. 391:L19-23,2008
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摘要：

对GRB 080319 B的光学和伽马射线观测使我们能够确定这一非凡爆发的相当完整的物理图像。数据表明，即时的光学和伽马射线光子产生在同一位置，但不同的辐射过程：同步加速器和同步加速器自康普顿，分别。爆发辐射是由一个超相对论源在距离爆炸中心10^{16.5} cm处产生的，该源以约500的洛伦兹因子运动。一个直接的推论是，在几十GeV时辐射出的能量一定比在~1 MeV时释放出的能量多10倍。假设GRB外流是重子流，而伽马射线源是激波加热的等离子体，那么驱动GRB 080319 B的喷流经过准直校正后的动能大于10^{52.3}尔格。早期余辉光发射的衰减（高达1 ks）是太快了，归因于反向冲击交叉的伽玛射线暴喷出物，但与预期的“大角度发射”的爆发过程中释放的一致。光学余辉通量从1 ks到10天的纯幂律衰减最自然地与传播到风状介质中的激波的（同步）发射相一致。然而，X射线余辉需要偏离标准的爆炸波模型。

英文摘要：

The optical and gamma-ray observations of GRB 080319B allow us to determine a fairly complete physical picture for this remarkable burst. The data indicate that the prompt optical and gamma-ray photons were produced at the same location but by different radiation processes: synchrotron and synchrotron self-Compton, respectively. The burst emission was produced at a distance of 10^{16.5} cm from the center of explosion by an ultra-relativistic source moving at Lorentz factor of ~500. A straightforward inference is that about 10 times more energy must have been radiated at tens of GeV than that released at ~1 MeV. Assuming that the GRB outflow was baryonic and that the gamma-ray source was shock-heated plasma, the collimation-corrected kinetic energy of the jet powering GRB 080319B was larger than 10^{52.3} erg. The decay of the early afterglow optical emission (up to 1 ks) is too fast to be attributed to the reverse shock crossing the GRB ejecta but is consistent with the expectations for the "large-angle emission" released during the burst. The pure power-law decay of the optical afterglow flux from 1 ks to 10 day is most naturally identified with the (synchrotron) emission from the shock propagating into a wind-like medium. However, the X-ray afterglow requires a departure from the standard blast-wave model.

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