Abstract
We discuss a new N-body simulation method for studying black hole binary dynamics. This method avoids previous numerical problems due to large mass ratios and trapped orbits with short periods. A treatment of relativistic effects is included when the associated time-scale becomes small. Preliminary results with up to N = 2.4 × 105 particles are obtained showing systematic eccentricity growth until the relativistic regime is reached, with subsequent coalescence in some cases.
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© 2003 Springer Science+Business Media Dordrecht
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Aarseth, S.J. (2003). Black Hole Binary Dynamics. In: Wickramasinghe, C., Burbidge, G., Narlikar, J. (eds) Fred Hoyle’s Universe. Springer, Dordrecht. https://doi.org/10.1007/978-94-017-1605-5_12
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DOI: https://doi.org/10.1007/978-94-017-1605-5_12
Publisher Name: Springer, Dordrecht
Print ISBN: 978-90-481-6339-7
Online ISBN: 978-94-017-1605-5
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