Abstract

Poster - Splinter SNR

Thursday, 12 September 2024, 15:30   (S14)

How do supernova remnants cool in the optical emission lines?

Ekaterina Makarenko, Stefanie Walch, Daniel Seifried
1. Institute of Physics, University of Cologne

Observed supernova remnants (SNRs) often interact with dense nearby molecular clouds. In these high-density environments, radiative losses are significant and can be observed in forbidden lines at optical wavelengths, especially for evolved SNRs. To model this interaction, we developed a post-processing module CESS (Cooling Emission in the optical band from Supernovae in (M)HD Simulations). This module uses the updated collision data from the MAPPINGS V code to produce realistic emission maps of simulated SNRs with 3D (magneto)hydrodynamic FLASH code in optical emission lines ([O III], [N II], [S II], Halpha, Hbeta). Our shock detection scheme shows that [S II] and [N II] emissions arise from the thin shell surrounding the SNR, while [O III], Halpha, and Hbeta originate from the volume-filling hot gas inside the SNR bubble. We find that the optical emission lines are affected by the SNR's complex structure and its projection on to the plane of the sky because the escaping line luminosity can be reduced by 10-80 per cent due to absorption along the line of sight.