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On The Maximum Mass of Stellar Black Holes | | Krzysztof Belczynski
; Tomasz Bulik
; Chris L. Fryer
; Ashley Ruiter
; Jorick S. Vink
; Jarrod R. Hurley
; | | Date: |
17 Apr 2009 | | Abstract: | We present the spectrum of compact object masses: neutron stars and black
holes that originate from single stars in different environments. In
particular, we show the dependence of maximum black hole mass on metallicity
and on some specific wind mass loss rates (e.g., Hurley et al. and Vink et
al.). We demonstrate that the highest mass black holes observed in the Galaxy
M_bh ~ 15 Msun in the high metallicity environment (Z=Zsun=0.02) can be
explained with stellar models and the wind mass loss rates adopted here. To
reach this conclusion it was required to set Luminous Blue Variable mass loss
rates at the level of ~ 0.0001 Msun/yr and to employ metallicity dependent
Wolf-Rayet winds. With the calibrated (on Galactic black hole mass
measurements) winds the maximum black hole mass predicted for moderate
metallicity (Z=0.3 Zsun=0.006) is M_bh,max = 30 Msun. This is a rather striking
finding as the mass of the most massive known stellar black hole is M_bh =
23-34 Msun and, in fact, it is located in a small star forming galaxy with
moderate metallicity. It is also predicted that in the very low (globular
cluster-like) metallicity environment the maximum black hole mass can be as
high as M_bh,max = 80 Msun (Z=0.01 Zsun=0.0002). We emphasize that our results
were obtained for single stars only and that binary interactions may alter the
predictions (e.g., accretion from a close companion) for maximum black hole
masses. This is strictly a proof-of-principle study which demonstrates that
stellar models can naturally explain even the most massive known stellar black
holes. | | Source: | arXiv, 0904.2784 | | Services: | Forum | Review | PDF | Favorites | |
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