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Improved methods for simulating nearly extremal binary black holes
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DOI：10.1088/0264-9381/32/10/105009.png)
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Abstract
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Astrophysical black holes could be nearly extremal (that is, rotating nearly as fast as possible); therefore, nearly extremal black holes could be among the binaries that current and future gravitational-wave observatories will detect. Predicting the gravitational waves emitted by merging black holes requires numerical-relativity simulations, but these simulations are especially challenging when one or both holes have mass m and spin S exceeding the Bowen-York limit of S/m(2) = 0.93. We present improved methods that enable us to simulate merging, nearly extremal black holes (i.e., black holes with S/m(2) > 0.93) more robustly and more efficiently. We use these methods to simulate an unequal-mass, precessing binary black hole (BBH) coalescence, where the larger black hole has S/m(2) = 0.99. We also use these methods to simulate a non-precessing BBH coalescence, where both black holes have S/m(2) = 0.994, nearly reaching the Novikov-Thorne upper bound for holes spun up by thin accretion disks. We demonstrate numerical convergence and estimate the numerical errors of the waveforms; we compare numerical waveforms from our simulations with post-Newtonian and effective-one-body waveforms; we compare the evolution of the black hole masses and spins with analytic predictions; and we explore the effect of increasing spin magnitude on the orbital dynamics (the so-called 'orbital hangup' effect).
Keywords:
numerical relativity
black holes
gravitational radiation
compact binaries
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