Transition from inspiral to plunge for eccentric equatorial Kerr orbits
نویسندگان
چکیده
منابع مشابه
Binary Black Holes Coalescence: Transition from Adiabatic Inspiral to Plunge
It seems likely that the first detection of gravitational waves with the LIGO/VIRGO/... interferometers will come from binary systems made of massive black holes of comparable masses, say with a total mass M ≃ 15M⊙ + 15M⊙. For such massive systems the gravitational-wave frequency at the last stable (circular) orbit (LSO) is very close to the location of the minimum of the detector’s noise spect...
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Combining recent techniques giving non-perturbative re-summed estimates of the damping and conservative parts of the two-body dynamics, we describe the transition between the adiabatic phase and the plunge, in coalescing binary black holes with comparable masses moving on quasi-circular orbits. We give initial dynamical data for numerical relativity investigations, with a fraction of an orbit l...
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There are three regimes of gravitational-radiation-reaction-induced inspiral for a compact body with mass m , in a circular, equatorial orbit around a Kerr black hole with mass M@m: ~i! the adiabatic inspiral regime, in which the body gradually descends through a sequence of circular, geodesic orbits; ~ii! a transition regime, near the innermost stable circular orbit ~isco!; ~iii! the plunge re...
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We present the first numerical calculation of the (local) metric perturbation produced by a small compact object moving on an eccentric equatorial geodesic around a Kerr black hole, accurate to first order in the mass ratio. The procedure starts by first solving the Teukolsky equation to obtain the Weyl scalar ψ4 using semi-analytical methods. The metric perturbation is then reconstructed from ...
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This paper presents the first calculation of the gravitational self-force on a small compact object on an eccentric equatorial orbit around a Kerr black hole to first order in the mass-ratio. That is the pointwise correction to the object’s equations of motion (both conservative and dissipative) due to its own gravitational field, which is treated as a linear perturbation to the background Kerr...
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ژورنال
عنوان ژورنال: Physical Review D
سال: 2003
ISSN: 0556-2821,1089-4918
DOI: 10.1103/physrevd.67.044004