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2004MNRAS.354..915M - Mon. Not. R. Astron. Soc., 354, 915-923 (2004/November-1)
Prompt γ-ray and early afterglow emission in the external shock model.
McMAHON E., KUMAR P. and PANAITESCU A.
Abstract (from CDS):
We have also calculated emission from the reverse shock for these ten bursts and find the flux in the optical band for more than half of these bursts to be between 9th and 12th magnitude at the deceleration time if the reverse shock microphysics parameters are the same as those found from afterglow modelling and the deceleration time is of the order of the burst duration. However, the cooling frequency in the reverse shock for most of these bursts is below the optical band, and therefore the observed flux decays rapidly with time (as ∼t–3) and is unobservable after a few deceleration times. It is also possible that the deceleration time is much larger than the burst duration, in which case we expect weak reverse shock emission.
Abstract Copyright: 2004 RAS
Journal keyword(s): radiation mechanisms: non-thermal - shock waves - methods: analytical - gamma-rays: bursts - gamma-rays: theory
Simbad objects: 16
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