paper

Swift GRB Afterglows and the Forward-Shock Model

arXiv:astro-ph/0612170 · doi:10.1111/j.1365-2966.2007.11956.x

Abstract

The X-ray light-curves of the GRB afterglows monitored by Swift display one to four phases of power-law decay. In chronological order they are: the burst tail, the "hump", the standard decay, and the post jet-break decay. The large-angle emission produced during the burst, but arriving at observer later, is consistent with the GRB tail decay for less than half of bursts. The forward-shock synchrotron emission from a very narrow jet (half-angle less than 1 deg) is consistent with the decay of 75 percent of GRB tails. The forward-shock inverse-Compton emission from a narrow jet that does not expand sideways also accommodates the decay of 80 percent of GRB tails. The X-ray light-curve hump can be attributed to an increasing kinetic energy per solid angle of the forward-shock region visible to the observer. This increase could be due to the emergence of the emission from an outflow seen from a location outside its opening. However, the correlations among the hump timing, flux, and decay index expected in this model are not confirmed by observations. Thus, the increase in the forward-shock kinetic energy is more likely caused by some incoming ejecta arriving at the shock during the afterglow phase. The jet interpretation for the burst tails and the energy injection scenario for the hump lead to a double-jet outflow structure consisting of a narrow GRB jet which precedes a wider afterglow outflow of lower kinetic energy per solid angle but higher total energy. (X-ray light-curves are shown for GRB 050416A, 050525A, 050717, 050721, 050724, 050730, 050802, 051109A, 060124, 060206, 060526).

accepted by MNRAS, 14 pages, 14 figures, additions: inverse-Compton emission for GRB tails (S2,fig3), implications for GRB efficiency (S3.1.3), achromatic breaks at ~1 hour (S4,fig10), GRB 060206 (S6,fig14)

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