Re-accretion of wind and supernova matter onto a central black hole.
| Název práce v češtině: | Reakrece hmoty hvězdných větrů a supernov na černou díru. |
|---|---|
| Název v anglickém jazyce: | Re-accretion of wind and supernova matter onto a central black hole. |
| Klíčová slova: | mezihvězdné bubliny|černé díry|supernovy|hydrodynamika|numerické metody |
| Klíčová slova anglicky: | ISM: bubbles|stars: black holes|supernovae: general|hydrodynamics|methods: numerical |
| Akademický rok vypsání: | 2023/2024 |
| Typ práce: | diplomová práce |
| Jazyk práce: | angličtina |
| Ústav: | Astronomický ústav UK (32-AUUK) |
| Vedoucí / školitel: | Mgr. Richard Wünsch, Ph.D. |
| Řešitel: | skrytý - zadáno a potvrzeno stud. odd. |
| Datum přihlášení: | 10.11.2023 |
| Datum zadání: | 14.11.2023 |
| Datum potvrzení stud. oddělením: | 14.04.2025 |
| Datum a čas obhajoby: | 10.06.2025 09:00 |
| Datum odevzdání elektronické podoby: | 29.04.2025 |
| Datum odevzdání tištěné podoby: | 30.04.2025 |
| Datum proběhlé obhajoby: | 10.06.2025 |
| Oponenti: | RNDr. Ondřej Chrenko, Ph.D. |
| Zásady pro vypracování |
| Stellar winds from massive stars lead to the formation of wind-blown bubbles composed of a cavity filled with wind matter and a dense and thin shell of swept-up interstellar matter (Weaver et al., 1977). The size of the bubble is determined by both, the energetics of the stellar wind and the pressure associated to the interstellar medium. After a massive star that ends its life as a core-collapse supernova (ccSN), a blast wave (BW) collides with the encompassing swept-up shell. The BW is typically unable to traverse the shell and thus the supernova remnant is confined to roughly the size of the wind-blown bubble (Tenorio-Tagle et al., 1990; Haid et al., 2016; Martinez-González et al., 2019). Not only that, but ccSNe leave behind either a neutron star, or a stellar mass black hole (BH). However, progenitors with masses above ~80 Solar masses end their lives as pair-instability supernovae, where the whole star is obliterated and thus stellar-mass BHs with masses in the interval 50-130 Solar masses were thought unlikely to exist_(e.g. Belczynski et al., 2016, Barack, L. et al. 2019). However, LIGO/VIRGO detections of gravitational waves originating from the coalescence of BHs with inferred masses falling in that interval (LIGO & Virgo Collaborations, 2020, 2021], Phys. Rev.Lett.125(2020), 101102), have challenged our understanding of stellar-mass BH formation and evolution.
The aim of this work is to investigate if the BHs left behind after the explosion of progenitors with masses close to ~80 Solar masses are able to efficiently re-accrete the wind and supernova matter within highly-pressurized wind-blown bubbles, and form black holes with masses in excess of 50 Solar masses. The student will use publicly available hydrodynamic code Flash (Fryxell et al., 2000) and home-grown modules that follow the evolution of wind-blown bubbles and supernova remnants (Wünsch et al., 2017), and calculate the gravitational potential associated to the gas and the central stellar-mass BH (Wünsch et al., 2018). |
| Seznam odborné literatury |
| Barack, L.; Cardoso, V.; Nissanke, S.; Sotiriou, T. P.; et al., 2019, CQGra 36, 143001
Belczynski K., Heger A., Gladysz W. et al. 2016 A&A 594, A97 Fryxell, B.; Olson, K.; Ricker, P. et al., 2000, ApJS, 131 273 Haid, S.; Walch, S.; Naab, T.; Seifried, D.; Mackey, J.; Gatto, A. 2016 MNRAS 460, 2962 Martínez-González, S.; Wünsch, R.; Silich, S.; Tenorio-Tagle, G.; Palouš, J.; Ferrara, A. 2019 ApJ 887, 198 Tenorio-Tagle, G.; Bodenheimer, P.; Franco, J.; Rozyczka, M. 1990, MNRAS, 244, 563 The LIGO Scientific Collaboration; the Virgo Collaboration; 2020 Phys. Rev. Lett. 125, 101102 The LIGO Scientific Collaboration ; the Virgo Collaboration ; the KAGRA Collaboration; 2023; arXiv:2111.03606 Weaver, R.; McCray, R.; Castor, J.; Shapiro, P.; Moore, R. 1977 ApJ 218, 377 Wünsch, R.; Palouš, J.; Tenorio-Tagle, G.; Ehlerová, S. 2017 ApJ 835, 60 Wünsch, R.; Walch, S.; Dinnbier, F.; Whitworth, A. 2018 MNRAS 475, 3393 |