Michela Mapelli
Published 2016-06-10Version 1
The runaway merger scenario is one of the most promising mechanisms to explain the formation of intermediate-mass black holes (IMBHs) in young dense star clusters (SCs). On the other hand, the massive stars that participate in the runaway merger lose mass by stellar winds. This effect is tremendously important, especially at high metallicity. We discuss N-body simulations of massive (~6x10^4 Msun) SCs, in which we added new recipes for stellar winds and supernova explosion at different metallicity. At solar metallicity, the mass of the final merger product spans from few solar masses up to ~30 Msun. At low metallicity (0.01-0.1 Zsun) the maximum remnant mass is ~250 Msun, in the range of IMBHs. A large fraction (~0.6) of the massive remnants are not ejected from the parent SC and acquire stellar or black hole companions. Finally, I discuss the importance of this result for gravitational wave detection.
Comments: 4 pages, 3 figures, 1 table, to appear in Memorie della SAIt (proceedings of the Modest 16 conference, 18-22 April 2016, Bologna, Italy)
H$_{2}$O Maser Pumping: The Effect of Quasi-Resonance Energy Transfer in Collisions between H$_2$ and H$_2$O Molecules
Are Super-Luminous supernovae and Long GRBs produced exclusively in young dense star clusters?
On the deceleration of Fanaroff-Riley Class I jets: mass loading of magnetized jets by stellar winds
![QR code for arXiv:1606.03370 [astro-ph.HE]](http://oss.arxitics.com/images/favicon.svg)