Surrogate models for precessing binary black hole simulations with unequal 
masses

Varma, Vijay; Field, Scott E.; Scheel, Mark A.; Blackman, Jonathan; Gerosa, Davide; Stein, Leo C.; Kidder, Lawrence E.; Pfeiffer, Harald

doi:10.1103/PhysRevResearch.1.033015

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学術論文

Surrogate models for precessing binary black hole simulations with unequal masses

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Pfeiffer, Harald
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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1905.09300.pdf
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PhysRevResearch.1.033015.pdf
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引用

Varma, V., Field, S. E., Scheel, M. A., Blackman, J., Gerosa, D., Stein, L. C., Kidder, L. E., & Pfeiffer, H. (2019). Surrogate models for precessing binary black hole simulations with unequal masses. Physical Review Research, 1:. doi:10.1103/PhysRevResearch.1.033015.

引用: https://hdl.handle.net/21.11116/0000-0004-3A82-8

要旨

Only numerical relativity simulations can capture the full complexities of
binary black hole mergers. These simulations, however, are prohibitively
expensive for direct data analysis applications such as parameter estimation.
We present two new fast and accurate surrogate models for the outputs of these
simulations: the first model, NRSur7dq4, predicts the gravitational waveform
and the second model, surfinBH7dq4, predicts the properties of the remnant
black hole. These models extend previous 7-dimensional, non-eccentric
precessing models to higher mass ratios, and have been trained against 1528
simulations with mass ratios $q\leq4$ and spin magnitudes $\chi_1,\chi_2 \leq
0.8$, with generic spin directions. The waveform model, NRSur7dq4, which begins
about 20 orbits before merger, includes all $\ell \leq 4$ spin-weighted
spherical harmonic modes, as well as the precession frame dynamics and spin
evolution of the black holes. The final black hole model, surfinBH7dq4, models
the mass, spin, and recoil kick velocity of the remnant black hole. In their
regime of validity, both models are shown to be more accurate than existing
models by at least an order of magnitude, with errors comparable to the
estimated errors in the numerical relativity simulations.