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arxiv: 2104.07052 · v2 · pith:XCKML53Cnew · submitted 2021-04-14 · 🌀 gr-qc

Comparing Remnant Properties from Horizon Data and Asymptotic Data in Numerical Relativity

Dante A. B. Iozzo , Neev Khera , Leo C. Stein , Keefe Mitman , Michael Boyle , Nils Deppe , Francois Hebert , Lawrence E. Kidder
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Jordan Moxon Harald P. Pfeiffer Mark A. Scheel Saul A. Teukolsky William Throwe
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classification 🌀 gr-qc
keywords remnantdatapropertiesasymptoticblackholehorizonnumerical
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We present a new study of remnant black hole properties from 13 binary black hole systems, numerically evolved using the Spectral Einstein Code. The mass, spin, and recoil velocity of each remnant were determined quasi-locally from apparent horizon data and asymptotically from Bondi data $(h, \psi_4, \psi_3, \psi_2, \psi_1)$ computed at future null infinity using SpECTRE's Cauchy characteristic evolution. We compare these independent measurements of the remnant properties in the bulk and on the boundary of the spacetime, giving insight into how well asymptotic data are able to reproduce local properties of the remnant black hole in numerical relativity. We also discuss the theoretical framework for connecting horizon quantities to asymptotic quantities and how it relates to our results. This study recommends a simple improvement to the recoil velocities reported in the Simulating eXtreme Spacetimes waveform catalog, provides an improvement to future surrogate remnant models, and offers new analysis techniques for evaluating the physical accuracy of numerical simulations.

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Cited by 4 Pith papers

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

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    Two new surrogate models, trained on NR simulations, predict remnant properties and eccentricity dynamics for nonspinning eccentric black hole binaries with q ≤ 4 and e < 0.23.

  4. Cusp Formation in Merging Black Hole Horizons

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    Numerical simulations of head-on black hole mergers reveal cusp formation on horizons, with mass and multipole moments behaving in ways that link initial and final black hole states via a phenomenological model.