On the existence of a reverse shock in magnetized GRB ejecta

Abstract

The role of magnetic fields in gamma-ray burst (GRB) flows remains controversial. The study of the early afterglow phases and, in particular, of the reverse shock dynamics and associated emission offers a promising probe of the magnetization of the ejecta. In this paper, we derive the conditions for the existence of a reverse shock in arbitrarily magnetized ejecta that decelerate and interact with the circumburst medium. Both constant and wind-like density profiles are considered. We show, in contrast to previous estimates, that ejecta with magnetization larger than unity are not crossed by a reverse shock for a large fraction of the parameter space relevant to GRB flows. Allowing for shell spreading, there is always a relativistic or mildly relativistic reverse shock forming in sigma_o < 0.3 ejecta. From this, we conclude that the paucity of optical flashes, believed to be a distinctive signature of a reverse shock, may be explained by the existence of dynamically important magnetic fields in the ejecta.

8 pages, 1 figure, A&A in press, small changes to match the accepted version

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Cited by in corpus (4)

• A statistical study of gamma-ray burst afterglows measured by the Swift Ultra-violet Optical Telescope
• Deceleration of arbitrarily magnetized GRB ejecta: the complete evolution
• Magnetohydrodynamic Effects in Propagating Relativistic Jets: Reverse Shock and Magnetic Acceleration
• An RMHD study of transition between prompt and afterglow GRB phases