Detecting the imprint of a kilonova or supernova \ in short GRB afterglows. (arXiv:1901.09220v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Guessoum_N/0/1/0/all/0/1">Nidhal Guessoum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zitouni_H/0/1/0/all/0/1">Hannachi Zitouni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mochkovitch_R/0/1/0/all/0/1">Robert Mochkovitch</a>
Short gamma-ray bursts result from mergers of two neutron stars or from
collapsars, but probably at a smaller rate. In the first case, a kilonova
occurs while in the second case a Type Ic supernova is expected. } {Even if
future observations of kilonovae in association with gravitational wave events
provide better data, detecting a kilonova during an afterglow follow-up would
remain useful for exploring the diversity of the kilonova phenomenon. As
supernovae produce a weaker gravitational signal, afterglow follow-up will be
the only possible method to find one. In this work, we identify the conditions
of the burst energy, external density, kilonova mass, supernova luminosity,
that are necessary for the detection of a kilonova or supernova in the
follow-up of short GRB afterglows.} {We have used a simple kilonova model to
obtain the peak luminosities and times as a function of mass, expansion
velocity and ejected matter opacity. Afterglow light curves are computed for a
uniform medium and a stellar wind, in the kilonova and supernova cases,
respectively.} {We represent, using diagrams of the burst kinetic energy vs.
density of the external medium, the domains where the kilonova or supernova at
maximum is brighter than the afterglow. %LEt{Please check I have retained your
intended meaning -> It’s OK
Short gamma-ray bursts result from mergers of two neutron stars or from
collapsars, but probably at a smaller rate. In the first case, a kilonova
occurs while in the second case a Type Ic supernova is expected. } {Even if
future observations of kilonovae in association with gravitational wave events
provide better data, detecting a kilonova during an afterglow follow-up would
remain useful for exploring the diversity of the kilonova phenomenon. As
supernovae produce a weaker gravitational signal, afterglow follow-up will be
the only possible method to find one. In this work, we identify the conditions
of the burst energy, external density, kilonova mass, supernova luminosity,
that are necessary for the detection of a kilonova or supernova in the
follow-up of short GRB afterglows.} {We have used a simple kilonova model to
obtain the peak luminosities and times as a function of mass, expansion
velocity and ejected matter opacity. Afterglow light curves are computed for a
uniform medium and a stellar wind, in the kilonova and supernova cases,
respectively.} {We represent, using diagrams of the burst kinetic energy vs.
density of the external medium, the domains where the kilonova or supernova at
maximum is brighter than the afterglow. %LEt{Please check I have retained your
intended meaning -> It’s OK
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