Please use this identifier to cite or link to this item:
Full metadata record
DC FieldValueLanguage
dc.contributor.authorO'Brien, Paul T.-
dc.contributor.authorWillingale, Richard-
dc.contributor.authorOsborne, Julian P.-
dc.contributor.authorGoad, Michael R.-
dc.contributor.authorPage, Kim L.-
dc.contributor.authorVaughan, Simon A.-
dc.contributor.authorRol, Evert-
dc.contributor.authorBeardmore, Andrew P.-
dc.contributor.authorGodet, Olivier-
dc.contributor.authorHurkett, C. P.-
dc.contributor.authorWells, Alan A.-
dc.contributor.authorZhang, B.-
dc.contributor.authorKobayashi, Shiho-
dc.contributor.authorBurrows, David N.-
dc.contributor.authorNousek, John A.-
dc.contributor.authorKennea, Jamie A.-
dc.contributor.authorFalcone, Abraham D.-
dc.contributor.authorGrupe, Dirk-
dc.contributor.authorGehrels, Neil-
dc.contributor.authorBarthelmy, Scott D.-
dc.contributor.authorCannizzo, J.-
dc.contributor.authorCummings, J. R.-
dc.contributor.authorHill, Joanne E.-
dc.contributor.authorKrimm, H.-
dc.contributor.authorChincarini, Guido-
dc.contributor.authorTagliaferri, Gianpiero-
dc.contributor.authorCampana, Sergio-
dc.contributor.authorMoretti, Alberto-
dc.contributor.authorGiommi, Paolo-
dc.contributor.authorPerri, M.-
dc.contributor.authorMangano, V.-
dc.contributor.authorLa Parola, V.-
dc.identifier.citationAstrophysical Journal, 2006, 647(2), pp.1213-1237.-
dc.description.abstractWe 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.-
dc.publisherIOP Science-
dc.rights© 2006. The American Astronomical Society. All rights reserved. Deposited with reference to the publisher's archiving policy available on the SHERPA/RomEO website.-
dc.subjectaccretion disks-
dc.subjectblack hole physics-
dc.subjectgamma rays: bursts-
dc.titleThe early X-ray emission from GRBs-
dc.relation.raeRAE 2007-
dc.relation.deptX-ray and Observational Astronomy-
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

Files in This Item:
File Description SizeFormat 
The early X-ray emission from GRBs.pdf1.84 MBAdobe PDFView/Open

Items in LRA are protected by copyright, with all rights reserved, unless otherwise indicated.