Re'em Sari, Tsvi Piran
Published 1999-01-10Version 1
We calculate the expected spectrum and light curves of the early afterglow. For short GRBs the peak of the afterglow will be delayed, typically, by a few dozens of seconds after the burst. The x-ray and gamma-ray characteristics of this delayed emission provide a way to discriminate between late internal shocks emission (part of the GRB) and the early afterglow signal. Detection of this delayed emission will prove the internal shock scenario as producing the GRB, and will pinpoint the initial Lorentz factor gamma_0. In the optical band, the dominant emission arises from the reverse shock. This shock, carries an energy comparable to that of the forward shock. It radiates this energy at much lower frequencies, producing a short optical flash of 15th magnitude or brighter.
Comments: 2 pages. Submitted to A&A, Proc. of Rome Conf. on Gamma-ray Bursts in the Afterglow Era
Constraints on the bulk Lorentz factor in the internal shock scenario for gamma-ray bursts
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