期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 448, 期 4, 页码 3248-3264出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv251
关键词
methods: numerical; stars: massive; supernovae: general; H II regions; ISM: supernova remnants
资金
- STFC
- Large Facilities Capital Fund of BIS
- University of Oxford
- Cosmocomp fellowship
- European Research Council under the European Community [306483, 291294]
- European Research Council under the European Unions [278594-GasAroundGalaxies]
- Marie Curie Training Network CosmoComp [PITN-GA-2009-238356]
- ANR BINGO project [ANR-08-BLAN-0316-01]
- Adrian Beecroft
- Oxford Martin School
- Agence Nationale de la Recherche (ANR) [ANR-08-BLAN-0316] Funding Source: Agence Nationale de la Recherche (ANR)
- STFC [ST/H008896/1, ST/F003110/1] Funding Source: UKRI
We present numerical simulations of a 15 M-circle dot star in a suite of idealized environments in order to quantify the amount of energy transmitted to the interstellar medium (ISM). We include models of stellar winds, UV photoionization and the subsequent supernova based on theoretical models and observations of stellar evolution. The system is simulated in 3D using RAMSES-RT, an Adaptive Mesh Refinement Radiation Hydrodynamics code. We find that stellar winds have a negligible impact on the system owing to their relatively low luminosity compared to the other processes. The main impact of photoionization is to reduce the density of the medium into which the supernova explodes, reducing the rate of radiative cooling of the subsequent supernova. Finally, we present a grid of models quantifying the energy and momentum of the system that can be used to motivate simulations of feedback in the ISM unable to fully resolve the processes discussed in this work.
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