Abstract
In this work we focus on the technical details of the numerical simulations of the non-thermal transient Swift J1644+57, whose emission is probably produced by a two- component jet powered by a tidal disruption event. In this context we provide details of the coupling between the relativistic hydrodynamic simulations and the radiative transfer code. First, we consider the technical demands of one-dimensional simulations of a fast relativistic jet, and show to what extent (for the same physical parameters of the model) do the computed light curves depend on the numerical parameters of the different codes employed. In the second part we explain the difficulties of computing light curves from axisymmetric two dimensonal simulations and discuss a procedure that yields an acceptable tradeoff between the computational cost and the quality of the results.
Highlights
Tidal disruption events (TDE) of stars by massive black holes [1, 2, 3] provide one of the ways to detect an inactive massive black hole in the center of a galaxy
One of the first attempts to explain the radio emission of Swift J1644+57 using one-dimensional models and relativistic hydrodynamic simulations[16] assumed that the emission is coming from the shocks that form when the jet interacts with the circumnuclear medium (CNM)
While the model was successful in explaining the first few weeks of SwJ1644 radio emission, it turns out that the long-term emission is not accounted for by a radio afterglow from a single ultrarelativistic, narrow jet
Summary
Tidal disruption events (TDE) of stars by massive black holes [1, 2, 3] provide one of the ways to detect an inactive massive black hole in the center of a galaxy. One of the first attempts to explain the radio emission of Swift J1644+57 using one-dimensional models and relativistic hydrodynamic simulations[16] assumed that the emission is coming from the shocks that form when the jet interacts with the circumnuclear medium (CNM). This model is more analogous to a GRB afterglow than to an AGN1. The late time rebrightening implies that additional energy is injected in the external shock months after the burst[14] This may happen if, for instance, the jTDE is accompanied by a powerful mildly relativistic component[18]2. The discussion and summary is given in the Section 4
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