Reakrece hmoty hvězdných větrů a supernov na černou díru.

Kománek, David

Massive stars which end their life as stellar mass black holes significantly reshape their surrounding interstellar medium (ISM) through fast stellar winds, ultraviolet ionizing radiation, and supernova ejecta. The black holes subsequently form within this modi- fied environment. In this thesis, we explore whether black holes can accrete a significant amount of gas from this environment to explain the origin of relatively massive black holes that have been recently observed by gravitational waves. We present hydrodynamic sim- ulations that incorporate key physical processes, including thermal conduction, radiative cooling, gravity, and radiation transport. We model the properties of interstellar bubbles across a broad parameter space, considering both scenarios where the progenitor star ends its life in a core-collapse supernova and those involving direct collapse into a black hole. Our results demonstrate that a supernova explosion heats the bubble interior so strongly that its cooling time becomes prohibitively long, making substantial accretion onto the black hole unlikely. The scenario with direct collapse seems to be, according to our results, more favorable for gas accretion from the stellar wind bubble. However, even in this case the models we were able to calculate did not result in a significant...

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