Cenko 2009 Swift最亮的几个暴都有jet break

主要内容:
说明喷流模型是对的, 其他没有jet break的可能是选择效应

精彩摘抄:
GRB 050820A, 从上到下分别是X射线, 光学, 和射电


GRB 060418
GRB 080319B

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Title:		The Collimation and Energetics of the Brightest Swift Gamma-Ray Bursts
Authors:		Cenko, S. B.; Frail, D. A.; Harrison, F. A.; Kulkarni, S. R.; Nakar, E.; Chandra, P.; Butler, N. R.; Fox, D. B.; Gal-Yam, A.; Kasliwal, M. M.; Kelemen, J.; Moon, D. -S.; Price, P. A.; Rau, A.; Soderberg, A. M.; Teplitz, H. I.; Werner, M. W.; Bock, D. C. -J.; Bloom, J. S.; Starr, D. A.; Filippenko, A. V.; Chevalier, R. A.; Gehrels, N.; Nousek, J. N.; Piran, T.
Publication:		eprint arXiv:0905.0690
Publication Date:		05/2009
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		Submitted to ApJ, comments welcome
Bibliographic Code:		2009arXiv0905.0690C

Abstract

Long-duration gamma-ray bursts (GRBs) are widely believed to be highly-collimated explosions (opening angle theta ~ 1-10 deg). As a result of this beaming factor, the true energy release from a GRB is usually several orders of magnitude smaller than the observed isotropic value. Measuring this opening angle, typically inferred from an achromatic steepening in the afterglow light curve (a "jet" break), has proven exceedingly difficult in the Swift era. Here we undertake a study of five of the brightest (in terms of the isotropic prompt gamma-ray energy release, E(gamma, iso)) GRBs in the Swift era to search for jet breaks and hence constrain the collimation-corrected energy release. We present multi-wavelength (radio through X-ray) observations of GRBs 050820A, 060418, and 080319B, and construct afterglow models to extract the opening angle and beaming-corrected energy release for all three events. Together with results from previous analyses of GRBs 050904 and 070125, we find evidence for an achromatic jet break in all five events, strongly supporting the canonical picture of GRBs as collimated explosions. The most natural explanation for the lack of observed jet breaks from most Swift GRBs is therefore selection effects. However, the opening angles for the events in our sample are larger than would be expected if all GRBs had a canonical energy release of ~ 10e51 erg. The total energy release we measure for those "hyper-energetic" (E(total) >~ 10e52 erg) events in our sample is large enough to start challenging models with a magnetar as the compact central remnant.

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