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O’Brien, P. T; Willingale, R; Osborne, J; Goad, M. R; Page, K. L; Vaughan, S; Rol, E; Beardmore, A; Godet, O; Hurkett, C. P; Wells, A; Zhang, B; Kobayashi, S; Burrows, D. N; Nousek, J. A; Kennea, J. A; Falcone, A; Grupe, D; Gehrels, N; Barthelmy, S; Cannizzo, J; Cummings, J; Hill, J. E; Krimm, H; Chincarini, G; Tagliaferri, G; Campana, S; Moretti, A; Giommi, P; Perri, M; Mangano, V; LaParola, V
The Astrophysical journal, 08/2006, Volume: 647, Issue: 2Journal Article
We present observations of the early X-ray emission for a sample of 40 gamma-ray bursts (GRBs) obtained using the Swift satellite, for which the narrow-field instruments were pointed at the burst within 10 minutes of the trigger. Using data from the Burst Alert Telescope and the X-Ray Telescope, we show that the X-ray light curve can be well described by an exponential that relaxes into a power law, often with flares superimposed. The transition time between the exponential and the power law provides a physically defined timescale for the burst duration. In most bursts, the power law breaks to a shallower decay within the first hour, and a late emission "hump" is observed, which can last for many hours. In other GRBs the hump is weak or absent. The observed variety in the shape of the early X-ray light curve can be explained as a combination of three components: prompt emission from the central engine, afterglow, and the late hump. In this scenario, afterglow emission begins during or soon after the burst, and the observed shape of the X-ray light curve depends on the relative strengths of the emission due to the central engine and that of the afterglow. There is a strong correlation such that those GRBs with stronger afterglow components have brighter early optical emission. The late emission hump can have a total fluence equivalent to that of the prompt phase. GRBs with the strongest late humps have weak or no X-ray flares.
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