A new numerical code for hydrodynamical 3D simulations of supernova remnants

Abstract

We develop a 3D hydrodynamical code written in C programming language to study the expansion of supernova remnants (SNRs) in the surrounding medium. It is based on the MUSCL-Hancock finite volume scheme with the HLLC Riemann solver. The code initiates the supernova remnant already in the Sedov phase and simulates hydrodynamics of the subsequent remnant expansion. The simulation is optimized for studies of large scale interaction of a supernova remnant with the interstellar medium (ISM). After a detailed description of the code, and three tests of hydrodynamics, we present the results for a single remnant expanding into a uniform and fractally structured ISM, as the first application of the code. The simulation of SNR expanding in a uniform medium is compared with the Sedov law of expansion and Sedov self-similar solution to density, velocity and pressure profiles. The results indicate that the simulation presented here reproduces well the hydrodynamics of the supernova remnant expansion and is very practical due to its simplicity and speed. The SNR evolution in fractal ISM shows that clumps disturb the blast wave and produce interference of bow shocks, resulting in turbulent motions and inhomogenities inside the remnant. [Project of the Serbian Ministry of Education, Science and Technological Development, Grant no. 176005: Emission nebulae: structure and evolution]

Keywords

• methods: numerical
• ism: supernova remnants