Exploring the small mass ratio binary black hole merger via Zeno’s dichotomy approach. (arXiv:2006.04818v1 [gr-qc])
<a href="http://arxiv.org/find/gr-qc/1/au:+Lousto_C/0/1/0/all/0/1">Carlos O. Lousto</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Healy_J/0/1/0/all/0/1">James Healy</a>
We perform a sequence of binary black hole simulations with increasingly
small mass ratios, reaching a 128:1 binary that displays 13 orbits before
merger. Based on a detailed convergence study of the $q=m_1/m_2=1/15$
nonspinning case, we apply additional mesh refinements levels on the smaller
hole horizon to reach the $q=1/32$, $q=1/64$, and $q=1/128$ cases. Roughly
linear strong computational scaling with $1/q$ is observed on 8-nodes
simulations. We compute the remnant properties of the merger; final mass, spin,
and recoil velocity. We also compute the gravitational waveforms, peak
frequency, amplitude, and luminosity. We compare those values with predictions
of the corresponding phenomenological formulas, reproducing the particle limit,
and we then use these new results to improve their fitting coefficients.
We perform a sequence of binary black hole simulations with increasingly
small mass ratios, reaching a 128:1 binary that displays 13 orbits before
merger. Based on a detailed convergence study of the $q=m_1/m_2=1/15$
nonspinning case, we apply additional mesh refinements levels on the smaller
hole horizon to reach the $q=1/32$, $q=1/64$, and $q=1/128$ cases. Roughly
linear strong computational scaling with $1/q$ is observed on 8-nodes
simulations. We compute the remnant properties of the merger; final mass, spin,
and recoil velocity. We also compute the gravitational waveforms, peak
frequency, amplitude, and luminosity. We compare those values with predictions
of the corresponding phenomenological formulas, reproducing the particle limit,
and we then use these new results to improve their fitting coefficients.
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