The Simulation of Superluminous Supernovae Using the M1 Approach for Radiation Transfer
Е. М. Урвачев, D. S. Shidlovski, Nozomu Tominaga, S. I. Glazyrin, С. И. Блинников
Abstract
Abstract Superluminous supernovae can be explained by the interaction of their ejecta with a dense circumstellar medium. The resulting shock boosts the radiative luminosity of the supernova by converting mechanical energy into radiative energy. Accurate modeling of the shock, which suffers high radiative losses, requires the use of radiation hydrodynamics. High-precision methods have a large computational cost, so approximations are generally used. In this paper, we describe the implementation of the M1 approximation of radiation transfer using the hydrodynamics code, front . Basic tests show good agreement with reference solutions and with results from other codes. Additional tests were undertaken to show some cases where the M1 method produces unphysical results, such as in the regions where the light beams intersect each other. Tests with outgoing rays are also presented to validate the use of the M1 approach in supernova simulations. Further, a simple initial model for a superluminous supernova was created to study the shock-interacting mechanism. It is shown that the M1 approach correctly reproduces both the bolometric light curve of the supernova in one-dimensional, spherically symmetric simulations, as well as the dynamics of the thin dense layer that arises in this scenario due to extreme radiative cooling. The thin layer is unstable in multidimensional simulations, but the perturbations do not drastically change the photosphere’s parameters at the beginning of the simulation and do not strongly affect the light curve during the first 50 days.