Speaker
Description
Core-collapse supernovae are one of the main producers of cosmic dust. Their remnants incorporate the perfect conditions for molecules to grow to dust grains, starting from a few hundred days after the explosion. However, the produced 0.01 to 1 solar masses of dust per supernova will eventually encounter the energetic reverse shock, while an even larger amount of pre-existing interstellar dust is at risk of destruction by the forward shock. Numerical studies estimate that the total dust destruction of the forward shock ranges somewhere between 0.3 to 70 solar masses, possibly turning supernovae into dust sinks rather than dust sources. In the last decades, the importance of constraining the dust destruction rate of supernova remnant shocks has become even more pressing since other dust sources such as asymptotic giant branch stars alone cannot explain observations of dusty galaxies at high redshift. To realistically study the destroyed interstellar dust mass of forward shocks, we perform new high-resolution 3D supernova remnant simulations with AREPO and the dust post-processing code PAPERBOATS, which includes various dust transport and destruction processes. Unlike previous studies, we consider several complex phenomena simultaneously: sputtering, grain-grain collisions, magnetic fields, and a turbulent surrounding interstellar medium that closely resembles observations and can lead to significant dust shielding in dense filaments. The supernova, which is then induced into the system, develops highly asymmetric forward and reverse shocks, similar to observations of young supernova remnants such as Cassiopeia A. By covering a wide parameter space of different dust grain species, interstellar medium densities, turbulence strength, temperatures, and magnetic field strengths, we are able to constrain the actual amount of dust destroyed by the forward shock, depending on the properties of the supernova explosion site.
