Dynamical ejecta synchrotron emission as possible contributor to the rebrightening of GRB170817A
In 2104.04537 we study the fast component of the dynamical ejecta from the numerical relativity simulations of binary neutrino star mergers, targeted to GW170817. We show that the fast component is present in most simulations and its properties have a complex dependency on the binary properties and the equation of state (EOS). Additionally we model the non-thermal, synchrotron emission for the dynamical ejecta expanding into and shocking the interstellar medium. We show that this kilonova afterglow provides a natural explanation for the recently detected X-ray rebrightening of the GRB170817, 1243 days after merger. This presents a new avenue to constrain the parameters of the binary and another addition to the multimessenger studies of binary neutrino star mergers. Our analysis suggests that among the targeted models considered, equal mass binaries with very soft EOS and disfavored.
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