Abstract

Contributed Talk - Splinter SNR

Tuesday, 10 September 2024, 15:45   (S14)

Connecting stellar and galactic scales of stellar feedback

Yvonne A. Fichtner [1], Jonathan Mackey [2], Luca Grassitelli [1], Emilio Romano-Díaz [1], Cristiano Porciani [1,3,4,5]
[1] Argelander-Institut für Astronomie, Auf dem Hügel 71, D-53121 Bonn, Germany [2] Dublin Institute for Advanced Studies, Astronomy and Astrophysics Section, DIAS Dunsink Observatory, Dublin D15 XR2R, Ireland [3] SISSA, International School for Advanced Studies, Via Bonomea 265, 34136 Trieste, TS, Italy [4] Dipartimento di Fisica – Sezione di Astronomia, Università di Trieste, Via Tiepolo 11, 34131 Trieste, Italy [5] IFPU, Institute for Fundamental Physics of the Universe, via Beirut 2, 34151 Trieste, Italy

As feedback is essential for the evolution of galaxies and given that stars are below the resolution limit in galaxy simulations, its impact needs to be included through sub-grid models. We study the impact of the sub-resolution circumstellar medium on the feedback available at resolved scales in these simulations. We compute a grid of 1D simulations of the circumstellar medium, variing the ambient density and the stellar model (including single and binary stars) across a range of initial masses for massive stars. We model the feedback from photoionisation, stellar winds and SNe, and calculate the energy that flows through spheres at different distances from the star. We find that SNe dominate the energy budget, but the pre-SN feedback is vital for the efficiency of the feedback. During the pre-SN phase, photoionisation and post-main-sequence winds are strong contributors to the feedback. The retained energy is nearly independent of metallicity at a small distance. At a distance of 5 pc, the energy is comparable to the injection of winds and SNe, while further away energy dissipation can decrease the energy substantially. The ambient density delays the arrival of energy at larger distances, and alters the ratio of thermal and kinetic energy.