GAMMA-RAY BURSTS IN THE FERMI ERA: THE SPECTRAL ENERGY DISTRIBUTION OF THE PROMPT EMISSION

被引：16
作者：
Massaro, F. [1 ]
Grindlay, J. E. [1 ]
Paggi, A. [2 ]
机构：
[1] Harvard Smithsonian Astrophys Observ, Cambridge, MA 02138 USA
[2] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy
来源：
ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 714卷 / 02期
关键词：
acceleration of particles; gamma-ray burst: general; radiation mechanisms: non-thermal; LOG-PARABOLIC SPECTRA; LARGE-AREA TELESCOPE; PARTICLE-ACCELERATION; ELECTRON ACCELERATION; COSMIC-RAYS; EVOLUTION; BEPPOSAX; MKN-501; BLAZARS; BAND;
D O I：
10.1088/2041-8205/714/2/L299
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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.
引用
收藏
页码：L299 / L302
页数：4
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