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General Relativity and Quantum Cosmology, gr-qc
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 $M \approx 10^6M_\odot$, and (iii) the SNR increases as the
initial eccentricity increases for $M=10^6M_\odot$. We also show that
incorporating the contribution from the higher multipole modes of gravitational
waves is crucial for enhancing the detection rate.
