Eccentric Binary Black Hole Simulations with Numerical Relativity
ORAL
Abstract
We perform a systematic study of eccentric orbiting nonspinning black hole binaries. We first make a technical study of the optimal full numerical techniques to apply to these studies. We choose different gauge parameters and Courant factors, $c=dx/dt$, and find an optimal value for it of 0.45. We also find the grid structure and global resolution that optimize accuracy and speed of current computational resources. With these choices we perform a study of the merger times $t_m$ as a function of eccentricity for configurations with comparable orbital energy content and find that they are well represented by the post-Newtonian factor $F(e)=(1+73e^2/24+37e^4/96)/(1-e^2)^{7/2}$ when merger times are normalized to their quasicircular values, i.e. $t_m(e)/t_m\approx F(e)$. We then perform a systematic coverage of five small-medium eccentricities up to $e\sim0.45$ and six mass ratios up to 8.5:1 producing a total of 30 simulations covering up to 25 orbits to merger to further model merger times and as a seed to a forthcoming new systematic catalog of gravitational waveforms from eccentric binary black holes to directly perform parameter estimations of gravitational waves events.
*The authors also gratefully acknowledge the National Science Foundation (NSF) for financial support from Grant PHY-2207920. Computational resources were also provided by the Blue Sky, Green Prairies, and White Lagoon clusters at the CCRG-Rochester Institute of Technology, which were supported by NSF grants No.AST-1028087, No.PHY-1229173, No.PHY-1726215, and No.PHY-2018420. This work used the ACCESS allocation TG-PHY060027N, founded by NSF, and project PHY20007 Frontera, an NSF-funded Petascale computing system at the Texas Advanced Computing Center (TACC).
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Publication: G.Ficarra and C.O.Lousto, ``Eccentric Binary Black Hole Simulations with Numerical Relativity,'' [arXiv:2409.18728 [gr-qc]].
Presenters
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Carlos O Lousto
- Rochester Institute of Technology