Abstract
GRB 130427A was the most luminous gamma-ray burst detected in the last 30 years. With an isotropic energy output of 8.5 × 10 53 erg and redshift of 0.34, it combined very high energetics with a relative proximity to Earth in an unprecedented way. Sensitive X-ray observatories such as XMM-Newton and Chandra have detected the afterglow of this event for a record-breaking baseline longer than 80 million seconds. The light curve displays a simple power-law over more than three decades in time. In this presentation, we explore the consequences of this result for a few models put forward so far to interpret GRB 130427A, and more in general the implication of this outcome in the context of the standard forward shock model.
Highlights
The most energetic gamma-ray bursts—events that release ∼1054 erg—are relatively rare, and are found typically when examining very large cosmological volumes and high redshifts
We explore the consequences of this result for a few models put forward so far to interpret GRB 130427A, and more in general the implication of this outcome in the context of the standard forward shock model
We have only taken the data from 47 ks into account in our analysis, because we are interested in the late X-ray afterglow; our analysis concentrates on the consistency between models and the late X-ray data
Summary
Massimiliano De Pasquale 1,2, *, Mathew Page 1 , David Alexander Kann 3 , Samantha R. Mullard Space Science Laboratory (University College London), Holmbury St. Mary, Dorking RH5 6NT, UK. Istituto Astrofisica Spaziale e Fisica Cosmica Palermo (INAF), Palermo, Via U. Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile. Millennium Institute of Astrophysics, Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile. Dark Cosmology Centre, Niels Bohr Institutet, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark. Istituto Astrofisica Spaziale e Fisica Cosmica di Bologna (INAF), Via P. Received: 31 August 2016; Accepted: 26 December 2016; Published: 16 January 2017
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