![formation of blackhole formation of blackhole](https://cdn.mos.cms.futurecdn.net/76whNPtMNQdtfiCFXn9CTF-1200-80.jpg)
Product of common envelope evolution, is also considered. Models, the extra mass loss that could occur in a close binary, the Presupernova structure on the initial mass of the helium star. We identify these as progenitors of Type IbĪnd, perhaps, Type Ic supernovae and investigate the dependence of the As a result, the final massesĬonverge to a narrow range of small values: 2.26-3.55 Msunįor all stars considered. Stripped of their envelopes, these stars are subject toĮfficient (mass-dependent) mass loss. Or, for the more massive stars, because they were subject to a strong Phase, probably because they were in a mass- exchanging binary system Their hydrogen envelopes, either before or early in their helium-burning We identify these objects as Wolf-Rayet stars that have lost Msun is followed through all stages of hydrostatic nuclearīurning. The evolution of helium stars with initial masses in the range 4-20 We also comment on the possibility of black-hole kicks and their effect on binaries. We discuss possible biases against the detection or formation of X-ray transients with low-mass black holes. We find no evidence for a gap at low values (3-5Msun) or for a peak at higher values (~7Msun) of black hole masses, but we argue that our black hole mass distribution for binaries is consistent with the current sample of measured black-hole masses in X-ray transients. The distributions are continuous and extend over a broad range.
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We also study the effects of the uncertainties in the explosion and unbinding energies for different progenitors. Wind mass-loss causes the black hole distribution to become flatter and limits the maximum possible black-hole mass (<10-15Msun). Our results are most sensitive to mass loss from winds which is even more important in close binaries. The compact remnant distribution is dominated by neutron stars in the mass range 1.2-1.6Msun and falls off exponentially at higher remnant masses. Thus, we are able to derive the binary black hole mass distribution. We examine how the calculated black-hole mass distributions are modified by (i) strong wind mass loss at different evolutionary stages of the progenitors, and (ii) the presence of close binary companions to the black-hole progenitors. We use the results of recent 2D simulations of core-collapse to obtain the relation between remnant and progenitor masses and fold it with an initial mass function for the progenitors. We derive the theoretical distribution function of black hole masses by studying the formation processes of black holes. Comment: 23 pages total (including 11 figures), submitted to ApJ We discuss the remaining uncertainties of this result and outline the consequences of our results for the understanding of the progenitor evolution of X-ray binaries and gamma-ray burst models. Correspondingly, the final remnant masses, which were computed by following the supernova evolution and fallback of material for a time scale of about one year, are between 1.2 and 10 solar masses. The results range from strong supernova explosions for the lower final masses to the direct collapse of the star into a black hole for the largest final mass. We then compute the evolution of all models through collapse and bounce.
![formation of blackhole formation of blackhole](https://4.bp.blogspot.com/-Hel_UtUirYk/UiQUYASQv-I/AAAAAAAAFpg/MSKSqyTiWpo/s640/Black-Hole-Formation3.jpg)
Although the iron core masses at collapse are generally larger for stars with larger final masses, they do not depend monotonically on the final stellar mass or even the C/O-core mass. Varying this mass loss rate by a factor 6 leads to stellar masses at collapse that range from 3.1 to 10.7 solar masses. We study its post-mass transfer evolution as a function of the Wolf-Rayet wind mass loss rate (which is currently not well constrained and will probably vary with initial metallicity of the star). After core hydrogen exhaustion, the star expands, loses most of its envelope by Roche lobe overflow, and becomes a Wolf-Rayet star. We present models for the complete life and death of a 60 solar mass star evolving in a close binary system, from the main sequence phase to the formation of a compact remnant and fallback of supernova debris.