We study the influence of astrophysical formation scenarios on the precessional dynamics of spinning black-hole binaries by the time they enter the observational window of second- and third-generation gravitational-wave detectors, such as Advanced LIGO/Virgo, LIGO-India, KAGRA, and the Einstein Telescope. Under the plausible assumption that tidal interactions are efficient at aligning the spins of few-solar mass black-hole progenitors with the orbital angular momentum, we find that black-hole spins should be expected to preferentially lie in a plane when they become detectable by gravitational-wave interferometers. This "resonant plane" is identified by the conditions ΔΦ=0 or ΔΦ=±180, where ΔΦ is the angle between the components of the black-hole spins in the plane orthogonal to the orbital angular momentum. If the angles ΔΦ can be accurately measured for a large sample of gravitational-wave detections, their distribution will constrain models of compact binary formation. In particular, it will tell us whether tidal interactions are efficient and whether a mechanism such as mass transfer, stellar winds, or supernovae can induce a mass-ratio reversal (so that the heavier black hole is produced by the initially lighter stellar progenitor). Therefore, our model offers a concrete observational link between gravitational-wave measurements and astrophysics. We also hope that it will stimulate further studies of precessional dynamics, gravitational-wave template placement, and parameter estimation for binaries locked in the resonant plane.

Gerosa, D., Kesden, M., Berti, E., O'Shaughnessy, R., Sperhake, U. (2013). Resonant-plane locking and spin alignment in stellar-mass black-hole binaries: A diagnostic of compact-binary formation. PHYSICAL REVIEW D, PARTICLES, FIELDS, GRAVITATION, AND COSMOLOGY, 87(10) [10.1103/PhysRevD.87.104028].

Resonant-plane locking and spin alignment in stellar-mass black-hole binaries: A diagnostic of compact-binary formation

Gerosa D;
2013

Abstract

We study the influence of astrophysical formation scenarios on the precessional dynamics of spinning black-hole binaries by the time they enter the observational window of second- and third-generation gravitational-wave detectors, such as Advanced LIGO/Virgo, LIGO-India, KAGRA, and the Einstein Telescope. Under the plausible assumption that tidal interactions are efficient at aligning the spins of few-solar mass black-hole progenitors with the orbital angular momentum, we find that black-hole spins should be expected to preferentially lie in a plane when they become detectable by gravitational-wave interferometers. This "resonant plane" is identified by the conditions ΔΦ=0 or ΔΦ=±180, where ΔΦ is the angle between the components of the black-hole spins in the plane orthogonal to the orbital angular momentum. If the angles ΔΦ can be accurately measured for a large sample of gravitational-wave detections, their distribution will constrain models of compact binary formation. In particular, it will tell us whether tidal interactions are efficient and whether a mechanism such as mass transfer, stellar winds, or supernovae can induce a mass-ratio reversal (so that the heavier black hole is produced by the initially lighter stellar progenitor). Therefore, our model offers a concrete observational link between gravitational-wave measurements and astrophysics. We also hope that it will stimulate further studies of precessional dynamics, gravitational-wave template placement, and parameter estimation for binaries locked in the resonant plane.
Articolo in rivista - Articolo scientifico
black holes, gravitational waves, general relativity, relativistic astrophysics
English
2013
87
10
104028
none
Gerosa, D., Kesden, M., Berti, E., O'Shaughnessy, R., Sperhake, U. (2013). Resonant-plane locking and spin alignment in stellar-mass black-hole binaries: A diagnostic of compact-binary formation. PHYSICAL REVIEW D, PARTICLES, FIELDS, GRAVITATION, AND COSMOLOGY, 87(10) [10.1103/PhysRevD.87.104028].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/325425
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