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The Fourth RIT binary black hole simulations catalog: Extension to Eccentric Orbits

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arxiv 2202.00018 v1 pith:6GBQOAQR submitted 2022-01-31 gr-qc astro-ph.GAastro-ph.HE

classification gr-qcastro-ph.GAastro-ph.HE
keywords catalogbinaryblackeccentricfourthholeleq1mass
verification ladder T0 review T1 audit T2 compute T3 formal
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abstract

This fourth release of the RIT public catalog of numerical relativity black-hole-binary waveforms \url{http://ccrg.rit.edu/~RITCatalog} consists of 1881 accurate simulations that include 446 precessing and 611 nonprecessing quasicircular/inspiraling binary systems with mass ratios $q=m_1/m_2$ in the range $1/128\leq q\leq1$ and individual spins up to $s/m^2=0.95$; and 824 in eccentric orbits in the range $0<e\leq1$. The catalog also provides initial parameters of the binary, trajectory information, peak radiation, and final remnant black hole properties. The waveforms are corrected for the center of mass drifting and are extrapolated to future null infinity. As an application of this waveform catalog we reanalyze all of the peak radiation and remnant properties to find new, simple, correlations among them, valid in the presence of eccentricity, for practical astrophysical usage.

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Cited by 7 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Unified remnant models for aligned-spin, precessing, and eccentric binary black hole mergers

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  4. Consistency of spin effects between numerical relativity and perturbation theory for inspiraling comparable-mass black hole binaries

    gr-qc 2025-10 conditional novelty 6.0 of 10

    Adiabatic point-particle black hole perturbation theory reproduces numerical-relativity spin effects in comparable-mass inspirals to within ~1%, so only small spin-dependent post-adiabatic corrections are needed.

  5. Time-frequency structure in the post-merger binary black hole gravitational wave signal

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    Post-merger signals from asymmetric black hole binaries develop extra time-frequency peaks for strong aligned spin and a broken sky symmetry for mild precessing spin, consistent with the horizon-geometry correlation idea.

  6. AthenaK simulations of the binary black hole merger GW150914

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    A new open-source GPU code, AthenaK, reproduces the GW150914 merger: remnant mass within 0.01%, spin within 0.02%, and waveform phase within about 0.35 radians of established simulations.

  7. Revisiting GW150914 with a non-planar, eccentric waveform model

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    Using a waveform model that includes both eccentricity and spin precession, the authors confirm GW150914 was a quasi-circular, slowly spinning black hole merger, with eccentricity below 0.08 at 15 Hz.

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