Spin misalignments of binary black holes produced in the isolated field channel
Abstract
We explore how the stellar evolution of binary black hole (BBH) progenitors determines the spin misalignments and precessional morphologies of BBHs near merger. Relevant aspects of stellar evolution include: (1) common envelope evolution, which brings the BBHs close enough together to merge through gravitational-wave emission, (2) stable mass transfer, which can reverse the mass ratio of the stellar progenitors and favor one librating morphology over another, (3) natal kicks which can source BBH misalignments even for initially aligned stellar progenitors, (4) tides which can align progenitors spin with their orbital angular momentum and synchronize the orbital and rotational angular velocities, and (5) stellar winds which can reduce the progenitor spins. We examine how the competing influences of these processes depend on the initial masses, spins, metallicities, and binary separations of the BBH progenitors and identify the portions of parameter space most likely to be associated with distinctive BBH spin precession when the BBHs enter the sensitivity band of gravitational-wave detectors. This research will help to interpret future discoveries of precessing BBHs.
M.K. is supported by NSF Grant No. PHY-1607031.- Publication:
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APS April Meeting Abstracts
- Pub Date:
- 2019
- Bibcode:
- 2019APS..APRR16005K