Kumar 2008 伽玛暴本身的辐射模型

主要内容:
一篇长文章，认为伽玛暴本身的同步辐射模型不能用，暴的时标导致内激波发生的距离很远，远于减速半径了。
认为同步自康普顿可以，参数空间大，还有jitter emission也可能可以，还有电子被持续加热也可能行.

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Title:		A general scheme for modeling gamma-ray burst prompt emission
Authors:		Kumar, Pawan; McMahon, Erin; Austin, UT
Publication:		eprint arXiv:0802.2704
Publication Date:		02/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		Published in MNRAS Jan 2008, 56 pages; MNRAS 384, 33, 2008
Bibliographic Code:		2008arXiv0802.2704K

Abstract

We describe a general method for modeling gamma-ray burst prompt emission. We find that for the burst to be produced via the synchrotron process unphysical conditions are required -- the distance of the source from the center of the explosion ($R_\gamma$) must be larger than $\sim 10^{17}$cm and the source Lorentz factor $\gta 10^3$; for such a high Lorentz factor the deceleration radius ($R_d$) is less than $R_\gamma$ even if the number density of particles in the surrounding medium is as small as $\sim 0.1$ cm$^{-3}$. The result, $R_\gamma > R_d$, is in contradiction with the early x-ray and optical afterglow data. The synchrotron-self-Compton (SSC) process fares much better. There is a large solution space for a typical GRB prompt emission to be produced via the SSC process. The prompt optical emission accompanying the burst is found to be very bright ($\lta$ 14 mag; for $z\sim2$) in the SSC model, which exceeds the observed flux (or upper limit) for most GRBs. Continuous acceleration of electrons can significantly reduce the optical flux and bring it down to the observed limits. (Abridged)

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