On the Maximum Mass of Stellar Black Holes

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On the Maximum Mass of Stellar Black Holes

FORMATION AND EVOLUTION OF BLACK HOLES Aspen Center for Physics 2010 Winter Conference on Astrophysics February 14{20, 2010 TITLE: On The Maximum Mass of Stellar Black Holes SPEAKER: Krzysztof Belczynski (LANL) We present the spectrum of compact object masses: neutron stars and black holes that originate from single stars in different environments. In particu- lar, we calculate 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.). Our calculations show that the highest mass black holes observed in the Galaxy Mbh = 15M 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 result we had to set Luminous Blue Variable mass loss rates at the level of dM=dt = 0:0001M =yr and to employ metallicity de- pendent Wolf-Rayet winds. With such winds, calibrated on Galactic black hole mass measurements, the maximum black hole mass obtained for moderate metallicity (Z=0.3 Zsun=0.006) is Mbh;max = 30M . This is a rather striking finding as the mass of the most massive known stellar black hole is Mbh = 23 − 34M and, in fact, it is located in a small star forming galaxy with moderate metallicity. We find that in the very low (globular cluster- like) metallicity environment the maximum black hole mass can be as high as Mbh;max = 80M (Z=0.01 Zsun=0.0002). We emphasize that our results were obtained for single stars only and that binary interactions may alter these maximum black hole masses (e.g., accretion from a close companion). This is strictly a proof-of-principle study which demonstrates that stellar models can naturally explain even the most massive known stellar black holes..

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