Minimum energy and the end of the inspiral in the post-Newtonian approximation
arXiv:1602.03134 · doi:10.1103/PhysRevD.95.064016
Abstract
The early inspiral phase of a compact binary coalescence is well modelled by the post-Newtonian (PN) approximation to the orbital energy and gravitational wave flux. The transition from the inspiral phase to the plunge can be defined by the minimum energy circular orbit (MECO). In the extreme mass-ratio limit, up to the highest PN order known, the PN energy equals the energy of the exact Kerr solution. However, for comparable-mass systems the MECO of the PN energy does not exist when bodies have large spins. By including the exact Kerr limit and recently published post-Newtonian terms we extract a well-defined minimum of the orbital energy beyond which the plunge or merger occurs. We study the hybrid condition for a number of cases of both black hole and neutron stars and compare to other commonly employed definitions. Our method can be used for any known order of the post-Newtonian series and enables the MECO condition to be used to define the end of the inspiral phase for highly spinning, comparable mass systems.
References in corpus (17)
- Observation of Gravitational Waves from a Binary Black Hole Merger
- GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence
- Tests of general relativity with GW150914
- Tidal Love numbers of neutron stars
- Binary Black Hole Mergers in the first Advanced LIGO Observing Run
- Comparison of post-Newtonian templates for compact binary inspiral signals in gravitational-wave detectors
- Post-1-Newtonian tidal effects in the gravitational waveform from binary inspirals
- Relativistic Measurements from Timing the Binary Pulsar PSR B1913+16
- Implementing a search for aligned-spin neutron star -- black hole systems with advanced ground based gravitational wave detectors
- Gravitational self-force correction to the innermost stable circular orbit of a Schwarzschild black hole
- Testing general relativity using golden black-hole binaries
- Cubic order spin effects in the dynamics and gravitational wave energy flux of compact object binaries
- Equivalence of ADM Hamiltonian and Effective Field Theory approaches at next-to-next-to-leading order spin1-spin2 coupling of binary inspirals
- Tidal deformation of a slowly rotating black hole
- Gravitational Self-Force Correction to the Innermost Stable Circular Equatorial Orbit of a Kerr Black Hole
- Conservative corrections to the innermost stable circular orbit (ISCO) of a Kerr black hole: a new gauge-invariant post-Newtonian ISCO condition, and the ISCO shift due to test-particle spin and the gravitational self-force
- Tidal deformations of spinning black holes in Bowen-York initial data
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