Post-Newtonian Dynamics in Dense Star Clusters: Formation, Masses, and Merger Rates of Highly-Eccentric Black Hole Binaries. (arXiv:1811.04926v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_C/0/1/0/all/0/1">Carl L. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amaro_Seoane_P/0/1/0/all/0/1">Pau Amaro-Seoane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatterjee_S/0/1/0/all/0/1">Sourav Chatterjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kremer_K/0/1/0/all/0/1">Kyle Kremer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rasio_F/0/1/0/all/0/1">Frederic A. Rasio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Samsing_J/0/1/0/all/0/1">Johan Samsing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ye_C/0/1/0/all/0/1">Claire S. Ye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zevin_M/0/1/0/all/0/1">Michael Zevin</a>
Using state-of-the-art dynamical simulations of globular clusters, including
radiation reaction during black hole encounters and a cosmological model of
star cluster formation, we create a realistic population of dynamically-formed
binary black hole mergers across cosmic space and time. We show that in the
local universe, 10% of these binaries form as the result of gravitational-wave
emission between unbound black holes during chaotic resonant encounters, with
roughly half of those events having eccentricities detectable by current
ground-based gravitational-wave detectors. The mergers that occur inside
clusters typically have lower masses than binaries that were ejected from the
cluster many Gyrs ago. Gravitational-wave captures from globular clusters
contribute 1-2 Gpc^-3 yr^-1 to the binary merger rate in the local universe,
increasing to ~10 Gpc^-3 yr^-1 at z~3. Finally, we discuss some of the
technical difficulties associated with post-Newtonian scattering encounters,
and how care must be taken when measuring the binary parameters during a
dynamical capture.
Using state-of-the-art dynamical simulations of globular clusters, including
radiation reaction during black hole encounters and a cosmological model of
star cluster formation, we create a realistic population of dynamically-formed
binary black hole mergers across cosmic space and time. We show that in the
local universe, 10% of these binaries form as the result of gravitational-wave
emission between unbound black holes during chaotic resonant encounters, with
roughly half of those events having eccentricities detectable by current
ground-based gravitational-wave detectors. The mergers that occur inside
clusters typically have lower masses than binaries that were ejected from the
cluster many Gyrs ago. Gravitational-wave captures from globular clusters
contribute 1-2 Gpc^-3 yr^-1 to the binary merger rate in the local universe,
increasing to ~10 Gpc^-3 yr^-1 at z~3. Finally, we discuss some of the
technical difficulties associated with post-Newtonian scattering encounters,
and how care must be taken when measuring the binary parameters during a
dynamical capture.
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