Kumar 2008 GRB080319B的逆康普顿解释

主要内容:
同步辐射产生光学，逆康普顿散射产生伽玛射线。不过假定了光学就是nu_m.
同时解释了余辉。

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文章信息:

· arXiv e-print (arXiv:0805.0144)

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Title:		What did we learn from gamma-ray burst 080319B ?
Authors:		Kumar, P.; Panaitescu, A.
Publication:		eprint arXiv:0805.0144
Publication Date:		05/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		5 pages, submitted to MNRAS
Bibliographic Code:		2008arXiv0805.0144K

Abstract

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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