MG15 - Talk detail

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Abstract

Radiation transport plays a crucial role in most high-energy astrophysical processes, such as black hole accretion disks, jets, pulsar winds, core-collapse supernovae and gamma-ray bursts. In some of these, for instance in the so-called shock breakouts that occur in supernovae when radiation-mediated shocks reach a star's photosphere, radiation is transported between optically-thick and optically-thin regions. Therefore, it is optimal to approach such problems using methods that are able to describe both regimes, which is not a trivial task, since that requires the handling of timescales that sometimes can differ in several orders of magnitude. Also, in most of these phenomena, matter dynamics is severely influenced by the presence of strong electromagnetic fields. We present in this work a numerical code applicable to radiation transfer problems in relativistic hydrodynamics and magnetohydrodynamics, which we have designed as an independent module to be included in the freely-available PLUTO code.

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Accepted

Yes

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Title

Abstract

X-ray flashes are frequently observed to follow the prompt emission of gamma-ray bursts. It has been recently proposed that these flares result from shock breakouts in binary-driven hypernovae. In this scenario, the plasma originated from the induced gravitational collapse of a neutron star reaches the photosphere of the surrounding supernova ejecta, thus emitting a burst of photons that is afterwards observed as a flare. In this presentation we show a series of hydrodynamical simulations of the interaction between an electron-positron plasma and a supernova ejecta, considering this model as a possible explanation for the X-ray flares observed in GRB 160625B.

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