Hydrodynamic simulations of dust destruction in supernova remnants


Following the example of previous studies, we make use of a public MHD code (AstroBEAR) to simulate the supernova ejecta environment. We adopt the "Cloud Crushing" model presented in Silvia et al, 2010, but refrain from using tracer particles to represent our dust grains. Instead, we have developed a "Dusty Grid" model based on a combination of approaches summarized by Haworth et al., 2016. Currently, we are working on two dust processing treatments: external treatment and internal treatment. A visualization of a preliminary test with external tracer particles is shown to the right.


To simulate the conditions within a supernova remnant, we make use of the publicly available MHD code AstroBEAR developed at the University of Rochester, USA. AstroBEAR is a parallelized, adaptive mesh refinement, 3D MHD code widely used in the astrophysics community. Our internal treatment approach aims to include dust processing directly into the MHD code and is supported by a collaboration with AstroBEAR developer Dr Erica Fogerty (Los Alamos National Laboratory, Los Alamos, USA).

The "Cloud Crushing" Model

Fig. 1 - The 'cloud crushing' model

The "Cloud Crushing" model is shown in Figure 1. We split the computational domain into a pre- and a post-shock region. Density, pressure, temperature, and velocity are calculated according to the Rankine-Hugoniot conditions across the shock front. A cloud or clump of denser gas which is assumed to hold the majority of the new dust (Biscaro and Cherchneff, 2016) is placed in the pre-shock medium.

The "Dusty Grid" Model

Unlike previous studies, we do not include dust in form of tracer particles. Instead, we introduce overlaying grids representing a distribution of dust bins. The dust is then transported between cells according to partial differential equations describing the advection and inter-bin transport equations describing the dust processing.

last updated 07 November 2018