2016/06/10 by Michela Mapelli, Mapelli, Michela
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Gamma-ray bursts and supernovae #High Energy Astrophysical Phenomena (astro-ph.HE) #Pulsars and Gravitational Waves Research #Solar and Stellar Astrophysics (astro-ph.SR)
paper · pdf · doi:10.48550/arxiv.1606.03370
openalex publication_date 2016/06/10 · openalex created_date 2020/12/07 · openalex updated_date 2026/07/28
The runaway merger scenario is one of the most promising mechanisms to\nexplain the formation of intermediate-mass black holes (IMBHs) in young dense\nstar clusters (SCs). On the other hand, the massive stars that participate in\nthe runaway merger lose mass by stellar winds. This effect is tremendously\nimportant, especially at high metallicity. We discuss N-body simulations of\nmassive (~6x104 Msun) SCs, in which we added new recipes for stellar winds and\nsupernova explosion at different metallicity. At solar metallicity, the mass of\nthe final merger product spans from few solar masses up to ~30 Msun. At low\nmetallicity (0.01-0.1 Zsun) the maximum remnant mass is ~250 Msun, in the range\nof IMBHs. A large fraction (~0.6) of the massive remnants are not ejected from\nthe parent SC and acquire stellar or black hole companions. Finally, I discuss\nthe importance of this result for gravitational wave detection.\n