Progenitors of core-collapse supernovae (SN) lose a significant fraction of their mass before explosion via stellar winds, circumstellar disks, or bipolar lobes. The kinetic energy of the SN ejecta may be partially converted into radiation, giving rise to luminous transients comparable to the luminosities of the actual SN. We study the hydrodynamics of collisions between expanding SN ejecta and circumstellar medium (CSM). We calculate the rate of deceleration as well as the behavior of density, pressure, expansion velocity and temperature structure in the interaction zone with various geometrical configurations and initial density structures of CSM. The theoretical conclusions of our models will help to improve the determination of SN progenitors properties and CSM density distribution.
Open European Journal on Variable Stars
- Pub Date:
- April 2019