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GRB 130831A: The Birth and Death of a Magnetar at z=0.5

Massimiliano De PasqualeUniversity College LondonS. R. OatesIstituto Astrofisica Spaziale Fisica Cosmica, Palermo, ItalyJ. L. RacusinCenter for Research and Exploration in Space Science And Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt MD 20771, USAД. А. КаннThringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, GermanyBing ZhangDepartment of Physics and Astronomy, University of Nevada Las Vegas, Las Vegas, USAA. PozanenkoSpace Research Institute (IKI), Moscow, RussiaA. VolnovaSpace Research Institute (IKI), Moscow, RussiaA. TrotterUniversity of North Carolina at Chapel Hill, Chapel Hill, North Carolina, USANathan R. FrankUniversity of North Carolina at Chapel Hill, Chapel Hill, North Carolina, USAAntonino CucchiaraCenter for Research and Exploration in Space Science And Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt MD 20771, USAE. TrojaCenter for Research and Exploration in Space Science And Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt MD 20771, USAB. SbarufattiPennsylvania State University, University Park, PA, USAN. ButlerArizona State University, Tempe, Arizona, USAS. SchulzeInstituto de Astrofsica, Facultad de Fsica, Pontificia Universidad Catlica de Chile, 306, Santiago 22, ChileZ. CanoCentre for Astrophysics and Cosmology, University of Iceland, Reykjavik, IcelandMathew J. PageIstituto Astrofisica Spaziale Fisica Cosmica, Palermo, ItalyA. J. Castro‐TiradoIstituto de Astrofisica de Andalucia (CSIC), Granada, SpainJ. GorosabelUniversity of the Basque CountryA. Y. LienCenter for Research and Exploration in Space Science And Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt MD 20771, USAO. FoxUniversity of California Berkeley, USAO. LittlejohnsArizona State University, Tempe, Arizona, USAJ. S. BloomUniversity of California Berkeley, USAJ. X. ProchaskaUniversity of California Santa Cruz, USAJ. A. de DiegoUniversity of California Santa Cruz, USAJ. González‐HernándezUniversidad Nacional Autonoma de Mexico, Ciudad de Mexico, MexicoM. G. RicherUniversidad Nacional Autonoma de Mexico, Ciudad de Mexico, MexicoC. Román-ZúñigaUniversidad Nacional Autônoma de MéxicoA. M. WatsonUniversidad Nacional Autonoma de Mexico, Ciudad de Mexico, MexicoN. GehrelsCenter for Research and Exploration in Space Science And Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt MD 20771, USASamuel Harvey MoseleyNASA Goddard Space-Flight CenterA. KutyrevCenter for Research and Exploration in Space Science And Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt MD 20771, USASilvia ZaneIstituto Astrofisica Spaziale Fisica Cosmica, Palermo, ItalyV. HoetteThe University of Chicago, IL, USAR. R. RussellThe University of Chicago, IL, USAV. RumyantsevCrimean Astrophysical Observatory, 98409, pgt. Nauchny, CrimeaE. KlunkoInstitute of Solar-Terrestrial Physics, Russian Academy of Sciences, 664033, p/o box 291; Lermontov st., 126a, Irkutsk, RussiaО. БурхоновUlugh Beg Astronomical Institute, 100052, 33 Astronomicheskaya str., Tashkent, UzbekistanA. A. BreeveldIstituto Astrofisica Spaziale Fisica Cosmica, Palermo, ItalyD. ReichartUniversity of North Carolina at Chapel Hill, Chapel Hill, North Carolina, USAJ. HaislipUniversity of North Carolina at Chapel Hill, Chapel Hill, North Carolina, USA

2015en

ABI

Annotatsiya

© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. We present observations of GRB 130831A and its afterglow obtained with Swift, Chandra, and multiple ground-based observatories. This burst shows an uncommon drop in the X-ray light curve at about 105 s after the trigger, with a decay slope of aX ≃ 7. The standard Forward Shock (FS) model offers no explanation for such a behaviour. Instead, a model in which a newly born magnetar outflow powers the early X-ray emission is found to be more viable. After the drop, the X-ray afterglow resumes its decay with a slope characteristic of FS emission. The optical emission, on the other hand, displays no clear break across the X-ray drop and its decay is consistent with that of the late X-rays; we thus believe that the optical and late X-ray emission are both FS. We model our data to derive the kinetic energy of the ejecta and, in conjunction with the study of SN 2013fu associated with GRB 130831A, we work out for the first time the energy break-down of a supernova with a central engine into non-relativistic ejecta, relativistic ejecta that power the afterglow, and emission from the magnetar outflow.

Mavzular

Gamma-ray bursts and supernovae Astronomy and Astrophysical Research

Identifikatorlar

DOI: 10.22323/1.233.0071

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