Contributed Talk - Splinter ISM

Thursday, 24 September 2020, 14:17   (virtual room F)

Emission from cooling supernova shocks in MHD simulations

E. I. Makarenko, S. Walch, S. D. Clarke, D. Seifried
I. Physics Institute, Department of Physics, University of Cologne

Each supernova (SN) injects $\sim 10^{51}$ erg into the interstellar medium (ISM). The blast wave shocks the gas and heats it up to 10$^{7}$ K; the gas subsequently cools by emitting radiation across the electromagnetic spectrum. Typically, about 70\% of the initially injected SN energy is lost by radiative cooling. Thus an understanding of the radiative losses is needed to understand the evolution of supernova remnants, and to allow for comparisons between simulations and observations. We present a post-processing module for the FLASH code which calculates the cooling radiation from shock-heated gas in different energy bands. Using modern collision excitation data from MAPPING V, we produce realistic maps of SNe emission, allowing comparisons to real observations of supernova remnants (SNRs) and testing observational diagnostic tools. Here we focus on optical line emission, arising from the interaction between the shock wave and dense gas, and on the use of optical line ratios for determining shock parameters.