Angular Momentum for Black Hole Binaries in Numerical Relativity
Abstract: The extensive catalog of waveforms, with details of binary black hole inspiral and merger, offer an opportunity to understand black hole interactions beyond the large separation regime. We envision a research program that focuses on the transfer of angular momentum from spin of the individual holes to the orbital angular momentum and the role of tidal coupling in the process. That analysis will require the formulation of an expression for the orbital angular momentum of a binary, an expression that is useful at small separations, since that regime is well out of the range of Newtonian approximations and is where tidal coupling should be most interesting. We report here such an expression, a binary orbital angular momentum based on numerical relativity results for quasi-circular orbits, that agrees remarkably well with a similar quantity constructed with particle-perturbation techniques for the Kerr geometry.
- SXS Collaboration, SXS Waveform Catalog https://data.black-holes.org/waveforms/catalog.html
- For a radiating binary of comparable masses there is no conserved mechanical energy, so no “ISCO” in the PP sense. For simplicity, we shall continue to use the term ISCO to mean the onset of the plunge. The actual time of the plunge can be well approximated from the SXS waveforms.
- The “initial” parameters of a model are the data fed into the initial solver. The SXS catalog also provides parameters at a “reference” time, after the early “junk” radiation has dissipated. For models 0161 and 0164, the differences are less than 10%.
- A. E. H. Love, Proc. R. Soc. Lond. A 82 (1909).
- Richard Price and Ritesh Bacchar, in preparation.
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