Simulating the circum-stellar environment of supernova and GRB progenitors by combining stellar evolution models and hydrodynamical code

TL;DR

This paper combines stellar evolution models with hydrodynamical simulations to study the circum-stellar environment of massive stars, aiming to better understand wind interactions and mass loss history.

Contribution

It introduces a method integrating stellar evolution outputs with hydrodynamical simulations to analyze circum-stellar media around massive stars.

Findings

Preliminary simulation results of the medium around a fast rotating star.

Comparison with observations to understand wind-ISM interactions.

Potential constraints on stellar evolution models from circum-stellar medium analysis.

Abstract

The medium around massive stars is strongly shaped by the stellar winds. Those winds depend on various stellar parameters (effective temperature, luminosity, chemical composition, rotation, ...), which are varying as a function of the time. Using the wind properties obtained by classical stellar evolution code allows for the multi- D hydrodynamical simulation of the circum-stellar medium accounting for the time variations of the wind. We present here the preliminary results of the simulation of the medium around a fast rotating star. Comparing the results of such simulations with the observed properties of the circum-stellar medium will allow to better understand the interactions of the stellar winds with the interstellar medium, and could give hints on the past history of the mass loss around massive stars, providing constraints for stellar models.