期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 459, 期 4, 页码 3432-3446出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw869
关键词
gravitational waves; methods: numerical; stars: black holes; stars: kinematics and dynamics; stars: mass-loss; galaxies: star clusters: general
资金
- CINECA Award [HP10C3ANJY]
- Italian Ministry of Education, University and Research (MIUR) [FIRB 2012 RBFR12PM1F]
- INAF [PRIN-2014-14]
- MERAC Foundation
The runaway collision scenario is one of the most promising mechanisms to explain the formation of intermediate-mass black holes (IMBHs) in young dense star clusters. On the other hand, the massive stars that participate in the runaway collisions lose mass by stellar winds. In this paper, we discuss new N-body simulations of massive (6.5 x 10(4) M-aS (TM)) star clusters, in which we added upgraded recipes for stellar winds and supernova explosion at different metallicity. We follow the evolution of the principal collision product (PCP), through dynamics and stellar evolution, till it forms a stellar remnant. At solar metallicity, the mass of the final merger product spans from few solar masses up to similar to 30 M-aS (TM). At low metallicity (0.01-0.1 Z(aS (TM))) the maximum remnant mass is similar to 250 M-aS (TM), in the range of IMBHs. A large fraction (similar to 0.6) of the PCPs are not ejected from the parent star cluster and acquire stellar or black hole (BH) companions. Most of the long-lived binaries hosting a PCP are BH-BH binaries. We discuss the importance of this result for gravitational wave detection.
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