Black hole spins in coalescing binary black holes

Abstract

The possible formation mechanisms of massive close binary black holes (BHs) that can merge in the Hubble time to produce powerful gravitational wave bursts detected during advanced LIGO O1 and O2 science runs include the evolution from field low-metallicity massive binaries, the dynamical formation in dense stellar clusters and primordial BHs. Different formation channels produce different source distributions of total masses $M_{\mathrm{tot}}$ and effective spins ${\chi }_{\mathrm{eff}}$ of coalescing binary BHs. Using a modified \textsc{bse} code, we carry out extensive population synthesis calculations of the expected effective spin and total mass distributions from the standard field massive binary formation channel for different metallicities of BH progenitors (from zero-metal Population III stars up to solar metal abundance), different initial rotations of the binary components, stellar wind mass loss prescription, different BH formation models and a range of common envelope efficiencies. The stellar rotation is treated in two-zone (core-envelope) approximation using the effective core-envelope coupling time and with an account of the tidal synchronization of stellar envelope rotation during the binary system evolution. The results of our simulations, convolved with the metallicity-dependent star-formation history, show that the total masses and effective spins of the merging binary black holes detected during LIGO O1-O2 runs but the heaviest one (GW170729) can be simultaneously reproduced by the adopted BH formation models. Noticeable effective spin of GW170729 requires additional fallback from the rotating stellar envelope.

18 pages, 11 figures, accepted to MNRAS after taking into account star-formation rate history for comparison of the calculated BH-BH coalescences with observed systems, LIGO/Virgo GWTC-1 sources added

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Cited by in corpus (28)

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• The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks
• Formation and Evolution of Primordial Black Hole Binaries in the Early Universe
• The origin of spin in binary black holes: Predicting the distributions of the main observables of Advanced LIGO
• GW190521 may be an intermediate mass ratio inspiral
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• Constraining the abundance of primordial black holes with gravitational lensing of gravitational waves at LIGO frequencies
• Small-scale structure of primordial black hole dark matter and its implications for accretion
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• Pathways for producing binary black holes with large misaligned spins in the isolated formation channel
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• Spins of black holes in coalescing compact binaries
• The impact of distant fly-bys on the rate of binary primordial black hole mergers
• Where to find Electromagnetic Wave Counterparts of stellar-mass binary black hole mergers?
• Wide nutation: binary black-hole spins repeatedly oscillating from full alignment to full anti-alignment
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• Spin-Orbit Misalignments in Tertiary-Induced Black-Hole Binary Mergers: Theoretical Analysis
• Possible Electromagnetic Phenomena during the Coalescence of Neutron Star-Black Hole Binary Systems
• Are the observed black hole mergers spins consistent with field binary progenitors?
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• Stripping of a neutron star in a close binary system in a pair with a black hole
• How many VHE gamma-ray binaries with young pulsars can be observed?
• Gravitational wave astronomy: astrophysical and cosmological inferences
• Empirical correlation between masses of black holes and Wolf-Rayet stars derived from their mass distributions in spectroscopic binaries
• Signatures of spin precession and nutation in isolated black-hole binaries