Massaro 2010 用对数抛物线拟合伽马暴的谱

主要内容:

把两边都取对数，再把包含对数的量当作自变量和因变量，就是抛物线。实际上就是说在对数图上伽马暴的谱比较像抛物线。
和一般用幂律拟合比较不同呃，不过他们说他们这么做还有理论依据。

精彩摘抄:

不同模型在MeV附近都差不多，高能地方就很不一样了。

估计这个模型不会成功，不是有暴的高能一直是很好的power law嘛

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Title:		Gamma-ray Bursts in the Fermi Era: The Spectral Energy Distribution of the Prompt Emission
Authors:		Massaro, F.; Grindlay, J. E.; Paggi, A.
Affiliation:		AA(Harvard-Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USA ), AB(Harvard-Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USA ), AC(Dipartimento di Fisica, Università di Roma Tor Vergata, Via della Ricerca Scientifica 1, I-00133 Rome, Italy)
Publication:		The Astrophysical Journal Letters, Volume 714, Issue 2, pp. L299-L302 (2010). (ApJL Homepage)
Publication Date:		05/2010
Origin:		IOP
ApJ Keywords:		acceleration of particles, gamma-ray burst: general, radiation mechanisms: non-thermal
DOI:		10.1088/2041-8205/714/2/L299
Bibliographic Code:		2010ApJ...714L.299M

Abstract

Gamma-ray bursts (GRBs) show evidence of different light curves, duration, afterglows, and host galaxies and explode within a wide redshift range. However, their spectral energy distributions (SEDs) appear to be very similar, showing a curved shape. Band et al. proposed a phenomenological description of the integrated spectral shape for the GRB prompt emission, the so-called Band function. In this Letter, we suggest an alternative scenario to explain the curved shape of GRB SEDs: the log-parabolic model. In comparison with the Band spectral shape our model is statistically favored because it fits the GRB spectra with one parameter less than the Band function and is motivated by a theoretical acceleration scenario. The new Fermi observations of GRBs will be crucial for disentangling these two models.

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