The central engine of GRB 130831A and the energy breakdown of a relativistic explosion

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dc.contributor.authorDe Pasquale, M.
dc.contributor.authorOates, S. R.
dc.contributor.authorRacusin, J. L.
dc.contributor.authorKann, D. A.
dc.contributor.authorZhang, B.
dc.contributor.authorPozanenko, A.
dc.contributor.authorVolnova, A. A.
dc.contributor.authorTrotter, A.
dc.contributor.authorFrank, N.
dc.contributor.authorCucchiara, A.
dc.contributor.authorTroja, E.
dc.contributor.authorSbarufatti, B.
dc.contributor.authorButler, N. R.
dc.contributor.authorSchulze, S.
dc.contributor.authorCano, Z.
dc.contributor.authorPage, M. J.
dc.contributor.authorCastro Tirado, A. J.
dc.contributor.authorGorosabel, J.
dc.contributor.authorLien, A.
dc.contributor.authorFox, O.
dc.contributor.authorLittlejohns, O.
dc.contributor.authorBloom, J. S.
dc.contributor.authorProchaska, J. X.
dc.contributor.authorde Diego, J. A.
dc.contributor.authorGonzalez, J.
dc.contributor.authorRicher, M. G.
dc.contributor.authorRoman Zuniga, C.
dc.contributor.authorWatson, A. M.
dc.contributor.authorGehrels, N.
dc.contributor.authorMoseley, H.
dc.contributor.authorKutyrev, A.
dc.contributor.authorZane, S.
dc.contributor.authorHoette, V.
dc.contributor.authorRussell, R. R.
dc.contributor.authorRumyantsev, V.
dc.contributor.authorKlunko, E.
dc.contributor.authorBurkhonov, O.
dc.contributor.authorBreeveld, A. A.
dc.contributor.authorReichart, D. E.
dc.contributor.authorHaislip, J. B.
dc.date.accessioned2024-01-10T12:43:32Z
dc.date.available2024-01-10T12:43:32Z
dc.date.issued2016
dc.description.abstractGamma-ray bursts (GRBs) are the most luminous explosions in the Universe, yet the nature and physical properties of their energy sources are far from understood. Very important clues, however, can be inferred by studying the afterglows of these events. We present optical and X-ray observations of GRB 130831A obtained by Swift, Chandra, Skynet, Reionization And Transients Infra-Red camera, Maidanak, International Scientific Optical-Observation Network, Nordic Optical Telescope, Liverpool Telescope and Gran Telescopio Canarias. This burst shows a steep drop in the X-ray light curve at similar to 10(5) s after the trigger, with a power-law decay index of a similar to 6. Such a rare behaviour cannot be explained by the standard forward shock (FS) model and indicates that the emission, up to the fast decay at 105 s, must be of 'internal origin', produced by a dissipation process within an ultrarelativistic outflow. We propose that the source of such an outflow, which must produce the X-ray flux for similar to 1 d in the cosmological rest frame, is a newly born magnetar or black hole. After the drop, the faint X-ray afterglow continues with a much shallower decay. The optical emission, on the other hand, shows no break across the X-ray steep decrease, and the late-time decays of both the X-ray and optical are consistent. Using both the X-ray and optical data, we show that the emission after similar to 10(5) s can be explained well by the FS model. We model our data to derive the kinetic energy of the ejecta and thus measure the efficiency of the central engine of a GRB with emission of internal origin visible for a long time. Furthermore, we break down the energy budget of this GRB into the prompt emission, the late internal dissipation, the kinetic energy of the relativistic ejecta, and compare it with the energy of the associated supernova, SN 2013 fu.
dc.description.funderRFBR
dc.description.funderUK Space Agency
dc.description.funderSpanish Ministry
dc.description.funderCONICYT-Chile FONDECYT
dc.description.funderBasal-CATA
dc.description.funderIniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo
dc.description.funderThuringer Landessternwarte Tautenburg
dc.description.funderMax-Planck Institut fur Extraterrestrische Physik
dc.description.funderIcelandic Research Fund
dc.description.funderNASA
dc.description.funderCONACyT
dc.description.funderUNAM PAPIIT
dc.description.funderUC MEXUS-CONACyT
dc.description.funderRobert Martin Ayers Sciences Fund
dc.description.funderDirect For Mathematical & Physical Scien
dc.description.funderScience and Technology Facilities Council
dc.fechaingreso.objetodigital2024-04-29
dc.format.extent16 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stv2280
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stv2280
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/77603
dc.identifier.wosidWOS:000368005900103
dc.information.autorucFísica;Schulze S;S/I;237742
dc.issue.numero1
dc.language.isoen
dc.nota.accesocontenido parcial
dc.pagina.final1042
dc.pagina.inicio1027
dc.publisherOXFORD UNIV PRESS
dc.revistaMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
dc.rightsacceso restringido
dc.subjectradiation mechanisms: non-thermal
dc.subjectshock waves
dc.subjectgamma-ray burst: general
dc.subjectgamma-ray burst: individual: GRB 130831A
dc.subjectstars: magnetars
dc.subjectGAMMA-RAY BURSTS
dc.subjectMAGNETAR CENTRAL ENGINE
dc.subjectCONFIDENCE-LIMITS
dc.subjectPROTO-MAGNETARS
dc.subjectDATA RELEASE
dc.subjectSWIFT
dc.subjectAFTERGLOW
dc.subjectEMISSION
dc.subjectCALIBRATION
dc.subjectACCRETION
dc.subject.ods07 Affordable and Clean Energy
dc.subject.odspa07 Energía asequible y no contaminante
dc.titleThe central engine of GRB 130831A and the energy breakdown of a relativistic explosion
dc.typeartículo
dc.volumen455
sipa.codpersvinculados237742
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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