期刊
CLASSICAL AND QUANTUM GRAVITY
卷 32, 期 10, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0264-9381/32/10/105009
关键词
numerical relativity; black holes; gravitational radiation; compact binaries
类别
资金
- Sherman Fairchild Foundation
- NSF at Caltech [PHY-1440083, AST-1333520]
- NSF at Cornell [PHY-1306125, AST-1333129]
- NSF at California State University Fullerton [PHY-1307489]
- California State University Fullerton Junior Faculty Research Grant
- NSF [PHY-0960291, NSF-1429873]
- NSF XSEDE network [TG-PHY990007N]
- Research Corporation for Science Advancement
- California State University Fullerton
- Canada Foundation for Innovation under Compute Canada
- Government of Ontario
- Ontario Research Fund-Research Excellence
- University of Toronto
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1333129, 1333520] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Physics [1404569, 1307489] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Physics [1429873] Funding Source: National Science Foundation
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).
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