Radiation hydrodynamical simulations of eruptive mass Loss from progenitors of Type Ibn/IIn supernovae

TL;DR

This study uses radiation hydrodynamical simulations to explore how energy injection from nuclear burning in massive stars can cause eruptive mass loss, forming dense circumstellar matter that influences supernova types.

Contribution

It introduces a parameterized model linking nuclear burning energy injection to eruptive mass loss, providing insights into pre-supernova outbursts and CSM formation.

Findings

Energy injection can reproduce observed pre-supernova outbursts.

Ejected mass and CSM properties depend on injection parameters.

Model explains formation of dense CSM for Type IIn supernovae.

Abstract

Observations suggest that some massive stars experience violent and eruptive mass loss associated with significant brightening that cannot be explained by hydrostatic stellar models. This event seemingly forms dense circumstellar matter (CSM). The mechanism of eruptive mass loss has not been fully explained. We focus on the fact that the timescale of nuclear burning gets shorter than the dynamical timescale of the envelope a few years before core collapse for some massive stars. To reveal the properties of the eruptive mass loss, we investigate its relation to the energy injection at the bottom of the envelope supplied by nuclear burning taking place inside the core. In this study, we do not specify the actual mechanism for transporting energy from the site of nuclear burning to the bottom of the envelope. Instead, we parameterize the amount of injected energy and the injection time and try to extract information on these parameters from comparisons with observations. We carried out 1-D radiation hydrodynamical simulations for progenitors of red, yellow, and blue supergiants, and Wolf-Rayet stars. We calculated the evolution of the progenitors with a public stellar evolution code. We obtain the light curve associated with the eruption, the amount of ejected mass, and the CSM distribution at the time of core-collapse. The energy injection at the bottom of the envelope of a massive star within a period shorter than the dynamical timescale of the envelope could reproduce some observed optical outbursts prior to the core-collapse and form the CSM, which can power an interaction supernova (SN) classified as type IIn.