Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 490, Issue 4, Pages 4991-5001Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz2902
Keywords
black hole physics; stars: kinematics and dynamics; stars: neutron; Galaxy: kinematics and dynamics; galaxies: kinematics and dynamics
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Funding
- CIERA post-doctoral fellowship at Northwestern University
- Black Hole Initiative at Harvard University
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Observations of black hole-neutron star (BH-NS) mergers via gravitational waves (GWs) are of great interest for their electromagnetic counterparts, such as short gamma-ray bursts, and could provide crucial information on the nature of BHs and the NS crust and magnetosphere. While no event has been confirmed, a recent possible detection of a BH-NS merger event by the LIGO-Virgo collaboration has attracted a lot of attention to these sources. In this second paper of the series, we follow-up our study of the dynamical evolution of triples composed of an inner BH-NS binary. In particular, we examine how the progenitor metallicity affects the characteristics of the BH-NS mergers in triples. We determine the distributions of masses, orbital parameters, and merger times, as a function of the progenitor metallicity and initial triple orbital distributions, and show that the typical eccentricity in the LIGO band is 10-210-1. We derive a merger rate range of BH-NS = 1.9 x 10-4-22 Gpc-3 yr-1, consistent the LIGO-Virgo upper limit. Finally, we study the expected spin-orbit misalignments of merging BH-NS binaries from this channel, and find that typically the effective spin distribution is peaked at.eff 0 with significant tails.
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