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dc.contributor.authorPage, M.
dc.contributor.authorDe Pasquale, Massımılıano
dc.contributor.authorOates, S.
dc.contributor.authorZane, S.
dc.contributor.authorWard, P.
dc.contributor.authorSchady, P.
dc.contributor.authorBreeveld, A.
dc.contributor.authorHOLLAND, S.
dc.contributor.authorKuin, P.
dc.contributor.authorStill, M.
dc.contributor.authorROMING, P.
dc.contributor.authorEvans, P.
dc.date.accessioned2021-03-04T09:37:38Z
dc.date.available2021-03-04T09:37:38Z
dc.date.issued2009
dc.identifier.citationDe Pasquale M., Evans P., Oates S., Page M., Zane S., Schady P., Breeveld A., HOLLAND S., Kuin P., Still M., et al., "Jet breaks at the end of the slow decline phase of Swift GRB light curves", MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, cilt.392, sa.1, ss.153-169, 2009
dc.identifier.issn0035-8711
dc.identifier.othervv_1032021
dc.identifier.otherav_691108d2-bf84-4524-a3cf-3fc4b1607a04
dc.identifier.urihttp://hdl.handle.net/20.500.12627/72820
dc.identifier.urihttps://doi.org/10.1111/j.1365-2966.2008.13990.x
dc.description.abstractThe Swift mission has discovered an intriguing feature of gamma-ray burst (GRBs) afterglows, a phase of shallow decline of the flux in the X-ray and optical light curves. This behaviour is typically attributed to energy injection into the burst ejecta. At some point this phase ends, resulting in a break in the light curve, which is commonly interpreted as the cessation of the energy injection. In a few cases, however, while breaks in the X-ray light curve are observed, optical emission continues its slow flux decline. This behaviour suggests a more complex scenario. In this paper, we present a model that invokes a double component outflow, in which narrowly collimated ejecta are responsible for the X-ray emission while a broad outflow is responsible for the optical emission. The narrow component can produce a jet break in the X-ray light curve at relatively early times, while the optical emission does not break due to its lower degree of collimation. In our model both components are subject to energy injection for the whole duration of the follow-up observations. We apply this model to GRBs with chromatic breaks, and we show how it might change the interpretation of the GRBs canonical light curve. We also study our model from a theoretical point of view, investigating the possible configurations of frequencies and the values of GRB physical parameters allowed in our model.
dc.language.isoeng
dc.subjectUzay bilimi
dc.subjectTemel Bilimler
dc.subjectASTRONOMİ VE ASTROFİZİK
dc.subjectAstronomi ve Astrofizik
dc.subjectFizik
dc.subjectTemel Bilimler (SCI)
dc.titleJet breaks at the end of the slow decline phase of Swift GRB light curves
dc.typeMakale
dc.relation.journalMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
dc.contributor.departmentUniversity Of London , ,
dc.identifier.volume392
dc.identifier.issue1
dc.identifier.startpage153
dc.identifier.endpage169
dc.contributor.firstauthorID103441


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