# Hydrodynamic simulations of mechanical stellar feedback in a molecular cloud formed by thermal instability

## TL;DR

This study uses 3D hydrodynamic simulations to explore how stellar winds and supernovae from stars of different masses influence the structure and evolution of a molecular cloud formed by thermal instability, revealing significant feedback effects.

## Contribution

It provides detailed simulations of stellar feedback in a molecular cloud, highlighting how different stellar masses impact cloud morphology and star formation potential.

## Key findings

- Massive stars create large cavities and channels in the cloud.
- Supernovae from massive stars disrupt the entire cloud structure.
- Cold material can be ejected and potentially form new stars.

## Abstract

We have used the AMR hydrodynamic code, MG, to perform 3D hydrodynamic simulations with self-gravity of stellar feedback in a spherical clumpy molecular cloud formed through the action of thermal instability. We simulate the interaction of the mechanical energy input from 15 Msun, 40 Msun, 60 Msun and 120 Msun stars into a 100 pc-diameter 16,500 Msun cloud with a roughly spherical morphology with randomly distributed high density condensations. The stellar winds are introduced using appropriate non-rotating Geneva stellar evolution models. In the 15 Msun star case, the wind has very little effect, spreading around a few neighbouring clumps before becoming overwhelmed by the cloud collapse. In contrast, in the 40 Msun, 60 Msun and 120 Msun star cases, the more powerful stellar winds create large cavities and carve channels through the cloud, breaking out into the surrounding tenuous medium during the wind phase and considerably altering the cloud structure. After 4.97 Myrs, 3.97 Myrs and 3.01 Myrs respectively, the massive stars explode as supernovae (SNe). The wind-sculpted surroundings considerably affect the evolution of these SN events as they both escape the cloud along wind-carved channels and sweep up remaining clumps of cloud/wind material. The `cloud' as a coherent structure does not survive the SN from any of these stars, but only in the 120 Msun case is the cold molecular material completely destabilised and returned to the unstable thermal phase. In the 40 Msun and 60 Msun cases, coherent clumps of cold material are ejected from the cloud by the SN, potentially capable of further star formation.