The 80 Ms follow-up of the X-ray afterglow of GRB 130427A challenges the standard forward shock model

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dc.contributor.authorDe Pasquale, M.
dc.contributor.authorPage, M. J.
dc.contributor.authorKann, D. A.
dc.contributor.authorOates, S. R.
dc.contributor.authorSchulze, S.
dc.contributor.authorZhang, B.
dc.contributor.authorCano, Z.
dc.contributor.authorGendre, B.
dc.contributor.authorMalesani, D.
dc.contributor.authorRossi, A.
dc.contributor.authorTroja, E.
dc.contributor.authorPiro, L.
dc.contributor.authorBoer, M.
dc.contributor.authorStratta, G.
dc.contributor.authorGehrels, N.
dc.date.accessioned2024-01-10T13:43:43Z
dc.date.available2024-01-10T13:43:43Z
dc.date.issued2016
dc.description.abstractGRB 130427A was the brightest gamma-ray burst detected in the last 30 yr. With an equivalent isotropic energy output of 8.5 x 10(53) erg and redshift z = 0.34, it uniquely combined very high energetics with a relative proximity to Earth. As a consequence, its X-ray afterglow has been detected by sensitive X-ray observatories such as XMM-Newton and Chandra for a record-breaking baseline longer than 80 million seconds. We present the X-ray light curve of this event over such an interval. The light curve shows a simple power-law decay with a slope alpha = 1.309 +/- 0.007 over more than three decades in time (47 ks-83 Ms). We discuss the consequences of this result for a few models proposed so far to interpret GRB 130427A, and more in general the significance of this outcome in the context of the standard forward shock model. We find that this model has difficulty in explaining our data, in both cases of constant density and stellar-wind circumburst media, and requires far-fetched values for the physical parameters involved.
dc.description.funderPRIN-INAF
dc.description.funderPremiale LBT
dc.description.funderNASA
dc.description.funderFIGARONet collaborative network
dc.description.funderAgence Nationale de la Recherche
dc.description.funderTLS Tautenburg
dc.description.funderIda
dc.description.funderInstrument Center for Danish Astrophysics (IDA)
dc.description.funderItalian Ministry of Education, University and Research (MIUR)
dc.description.funderUK Space Agency
dc.description.funderSpanish Ministry
dc.description.funderIcelandic Research Fund (IRF)
dc.fechaingreso.objetodigital2024-04-29
dc.format.extent12 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stw1704
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stw1704
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/78738
dc.identifier.wosidWOS:000383516700112
dc.information.autorucFísica;Schulze S;S/I;237742
dc.issue.numero1
dc.language.isoen
dc.nota.accesocontenido parcial
dc.pagina.final1122
dc.pagina.inicio1111
dc.publisherOXFORD UNIV PRESS
dc.revistaMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
dc.rightsacceso restringido
dc.subjectgamma-ray burst: general
dc.subjectgamma-ray burst: individual: GRB 130427A
dc.subjectLIGHT CURVES
dc.subjectBURST AFTERGLOWS
dc.subjectCENTRAL ENGINE
dc.subjectVIEWING ANGLE
dc.subjectJET BREAKS
dc.subjectBROAD-BAND
dc.subjectSWIFT
dc.subjectSUPERNOVAE
dc.subjectMAGNETAR
dc.subjectENERGY
dc.subject.ods07 Affordable and Clean Energy
dc.subject.odspa07 Energía asequible y no contaminante
dc.titleThe 80 Ms follow-up of the X-ray afterglow of GRB 130427A challenges the standard forward shock model
dc.typeartículo
dc.volumen462
sipa.codpersvinculados237742
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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