Supernova Remnants and Supernova Feedback
Abstract
Supernova (SN) is a major feedback mechanism driving large-scale turbulence in the interstellar medium (ISM), which regulates star formation in galaxies. In recent years, it has become possible to directly simulate SN feedback in realistic multiphase ISM in full three dimensions with high resolution. Although there is an emerging consensus from these theoretical works on the evolution of supernova remnants (SNRs) and the momentum/energy input from a SN event to the ISM, observational constraints are still lacking and necessary to validate the theoretical understanding. In this presentation, we review the observations of SNRs in radiative phase in the Milky Way. There are eight SNRs where we can observe fast-expanding radiative shells in HI 21 cm line. The shell momentum is in the range of (0.5-4.5)×10^5 M⊙ km/s. Some of the SNRs are core-collapse SNRs interacting with molecular clouds, and they provide a template for the coupling of SN explosion energy and momentum to the inhomogeneous ISM. In two SNRs (W44 and IC 443), expanding molecular shells with momentum comparable to that of the atomic SNR shells have been also observed. We compare the observed momentum and kinetic/thermal energy of these eight SNRs with the results from 1D numerical simulations and discuss the implications.
- Publication:
-
Supernova Remnants: An Odyssey in Space after Stellar Death II
- Pub Date:
- June 2019
- Bibcode:
- 2019sros.confE.178K