Anderson 2014 GRB 130427A的早期射电余辉观测

主要内容:
说第一个是反向激波，第二个是外激波。第一个peak是反向激波nu_a穿过射电频率的时候。

精彩摘抄:
红色的点是AMI新观测的，包括早期的一个上升。

文章信息:

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Title:		Probing the Bright Radio Flare and Afterglow of GRB 130427A with the Arcminute Microkelvin Imager
Authors:		Anderson, G. E.; van der Horst, A. J.; Staley, T. D.; Fender, R. P.; Wijers, R. A. M. J.; Scaife, A. M. M.; Rumsey, C.;Titterington, D. J.; Rowlinson, A.; Saunders, R. D. E.
Publication:		eprint arXiv:1403.2217
Publication Date:		03/2014
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		Accepted for publication in MNRAS
Bibliographic Code:		2014arXiv1403.2217A

Abstract

We present one of the best sampled early time light curves of a gamma-ray burst (GRB) at radio wavelengths. Using the Arcminute Mircrokelvin Imager (AMI) we observed GRB 130427A at the central frequency of 15.7 GHz between 0.36 and 59.32 days post-burst. These results yield one of the earliest radio detections of a GRB and demonstrate a clear rise in flux less than one day after the gamma-ray trigger followed by a rapid decline. This early time radio emission probably originates in the GRB reverse shock so our AMI light curve reveals the first ever confirmed detection of a reverse shock peak in the radio domain. At later times (about 3.2 days post-burst) the rate of decline decreases, indicating that the forward shock component has begun to dominate the light-curve. Comparisons of the AMI light curve with modelling conducted by Perley et al. show that the most likely explanation of the early time 15.7 GHz peak is caused by the self-absorption turn-over frequency, rather than the peak frequency, of the reverse shock moving through the observing bands.

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