Gravitational wave emission under general parametrized metric from extreme mass ratio inspirals. (arXiv:1812.04185v1 [gr-qc])
<a href="http://arxiv.org/find/gr-qc/1/au:+Xin_S/0/1/0/all/0/1">Shuo Xin</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Han_W/0/1/0/all/0/1">Wen-Biao Han</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Yang_S/0/1/0/all/0/1">Shu-Cheng Yang</a>
Future space-borne interferometers will be able to detect gravitational waves
at $10^{-3}$ to $10^{-1}$ Hz. At this band extreme-mass-ratio inspirals (EMRIs)
can be promising gravitational wave sources. In this paper, we investigate
possibility of testing Kerr hypothesis against a parametrized non-Kerr metric
by matching EMRI signals. However, EMRIs from either equatorial orbits or
inclined orbits suffer from the “confusion problem”. Our results show that,
within the time scale before radiation flux plays an important role, small and
moderate deviations from the Kerr spacetime($|delta_i|<1$) can be discerned
only when spin parameter is high. In most cases, the EMRI waveforms related
with a non-Kerr metric can be mimicked by the waveform templates produced with
a Kerr black hole.
Future space-borne interferometers will be able to detect gravitational waves
at $10^{-3}$ to $10^{-1}$ Hz. At this band extreme-mass-ratio inspirals (EMRIs)
can be promising gravitational wave sources. In this paper, we investigate
possibility of testing Kerr hypothesis against a parametrized non-Kerr metric
by matching EMRI signals. However, EMRIs from either equatorial orbits or
inclined orbits suffer from the “confusion problem”. Our results show that,
within the time scale before radiation flux plays an important role, small and
moderate deviations from the Kerr spacetime($|delta_i|<1$) can be discerned
only when spin parameter is high. In most cases, the EMRI waveforms related
with a non-Kerr metric can be mimicked by the waveform templates produced with
a Kerr black hole.
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