Extreme mass ratio inspirals on the equatorial plane in the adiabatic order

Abstract

We compute gravitational waves from inspiraling stellar-mass compact objects on the equatorial plane of a massive spinning black hole (BH). Our inspiral orbits are computed by taking into account the adiabatic change of orbital parameters due to gravitational radiation in the lowest order in mass ratio. We employ an interpolation method to compute the adiabatic change at arbitrary points inside the region of orbital parameter space computed in advance. Using the obtained inspiral orbits and associated gravitational waves, we compute power spectra of gravitational waves and the signal-to-noise ratio (SNR) for several values of the BH spin, the masses of the binary, and the initial orbital eccentricity during a hypothetical three-yrs LISA observation before final plunge. We find that (i) the SNR increases as the BH spin and the mass of the compact object increase for the BH mass $M \agt 10^6M_\odot$, (ii) the SNR has a maximum for $M\approx 10^6{M}_{\odot }$, and (iii) the SNR increases as the initial eccentricity increases for $M=10^6{M}_{\odot }$. We also show that incorporating the contribution from the higher multipole modes of gravitational waves is crucial for enhancing the detection rate.

18 pages, 18 figures, published in Phys. Rev. D, supplementary data files available at https://sites.google.com/view/bhpc1996/home

References in corpus (19)

• Gravitational-wave sensitivity curves
• Comparison of post-Newtonian templates for compact binary inspiral signals in gravitational-wave detectors
• Two timescale analysis of extreme mass ratio inspirals in Kerr. I. Orbital Motion
• Gravitational wave snapshots of generic extreme mass ratio inspirals
• Faithful Effective-One-Body waveforms of small-mass-ratio coalescing black-hole binaries
• Comparing Effective-One-Body gravitational waveforms to accurate numerical data
• Osculating orbits in Schwarzschild spacetime, with an application to extreme mass-ratio inspirals
• Gravitational Waves from a Particle in Circular Orbits around a Schwarzschild Black Hole to the 22nd Post-Newtonian Order
• Extreme Mass-Ratio Inspirals in the Effective-One-Body Approach: Quasi-Circular, Equatorial Orbits around a Spinning Black Hole
• Computing inspirals in Kerr in the adiabatic regime. I. The scalar case
• An Efficient Numerical Method for Computing Gravitational Waves Induced by a Particle Moving on Eccentric Inclined Orbits around a Kerr Black Hole
• Forced motion near black holes
• Gravitational Waves from a Particle in Circular Orbits around a Rotating Black Hole to the 11th Post-Newtonian Order
• Calculation of radiation reaction effect on orbital parameters in Kerr spacetime
• Linear-in-mass-ratio contribution to spin precession and tidal invariants in Schwarzschild spacetime at very high post-Newtonian order
• Gravitational-wave flux for a particle orbiting a Kerr black hole to 20th post-Newtonian order: a numerical approach
• Impact of the second order self-forces on the dephasing of the gravitational waves from quasi-circular extreme mass-ratio inspirals
• Verifying black hole orbits with gravitational spectroscopy
• Note on Accuracy of the Post-Newtonian Approximation for Extreme-Mass Ratio Inspirals: Retrograde Orbits