Gravitational wave snapshots of generic extreme mass ratio inspirals
184 citations recorded by the source corpus.
Using black hole perturbation theory, we calculate the gravitational waves produced by test particles moving on bound geodesic orbits about rotating black holes. The orbits we consider are generic--simultaneously eccentric and inclined. The waves can be described as having radial, polar, and azimuthal ''voices,'' each of which can be made to dominate by varying eccentricity and inclination. Although each voice is generally apparent in the waveform, the radial voice is prone to overpowering the others. We also compute the radiative fluxes of energy and axial angular momentum at infinity and through the event horizon. These fluxes, coupled to a prescription for the radiative evolution of the Carter constant, will be used in future work to adiabatically evolve through a sequence of generic orbits. This will enable the calculation of inspiral waveforms that, while lacking certain important features, will approximate those expected from astrophysical extreme mass ratio captures sufficiently well to aid development of measurement algorithms on a relatively short time scale.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/ebc17fcd3afa9929120d4f4fd033ee98a168e04b
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In Astronomy and Astrophysics
Citations in the corpus
- Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime (2012, background): “However, the solution of this equation is computationally expensive, and results have only recently been obtained for a selection of generic orbits (Drasco and Hughes, 2006).”
- Two timescale analysis of extreme mass ratio inspirals in Kerr. I. Orbital Motion (2008, background): “[32] S. Babak, H. Fang, J. R. Gair, K. Glampedakis, and S. A. Hughes, “’Kludge’ gravitational waveforms for a test-body orbiting a Kerr black hole”, Phys.”
- Black hole perturbation theory and gravitational self-force (2021, methodology): “[57, 58, 65], finding the frequencies and angle variables by directly solving the geodesic equation.”
- The Motion of Point Particles in Curved Spacetime (2004, methodology): “In the hope of achieving similar success in the context of the self-force, considerable work has been done to formulate a similar approximation for the case of an extreme-mass-ratio inspiral [124, 125, 126, 98, 61, 62, 159, 158, 78, 128, 94].”
- The Motion of Point Particles in Curved Spacetime (2003, methodology): “In the hope of achieving similar success in the context of the self-force, considerable work has been done to formulate a similar approximation for the case of an extreme-mass-ratio inspiral [124, 125, 126, 98, 61, 62, 159, 158, 78, 128, 94].”