Adiabatic waveforms from extreme-mass-ratio inspirals: an analytical approach. (arXiv:2111.05288v2 [gr-qc] UPDATED)
<a href="http://arxiv.org/find/gr-qc/1/au:+Isoyama_S/0/1/0/all/0/1">Soichiro Isoyama</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Fujita_R/0/1/0/all/0/1">Ryuichi Fujita</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Chua_A/0/1/0/all/0/1">Alvin J. K. Chua</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Nakano_H/0/1/0/all/0/1">Hiroyuki Nakano</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Pound_A/0/1/0/all/0/1">Adam Pound</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Sago_N/0/1/0/all/0/1">Norichika Sago</a>
Scientific analysis for the gravitational-wave detector LISA will require
theoretical waveforms from extreme-mass-ratio inspirals (EMRIs) that
extensively cover all possible orbital and spin configurations around
astrophysical Kerr black holes. However, on-the-fly calculations of these
waveforms have not yet overcome the high dimensionality of the parameter space.
To confront this challenge, we present a user-ready EMRI waveform model for
generic (eccentric and inclined) orbits in Kerr spacetime, using an analytical
self-force approach. Our model accurately covers all EMRIs with arbitrary
inclination and black hole spin, up to modest eccentricity ($lesssim 0.3$) and
separation ($gtrsim2$–$10M$ from the last stable orbit). In that regime, our
waveforms are accurate at the leading `adiabatic’ order, and they approximately
capture transient self-force resonances that significantly impact the
gravitational-wave phase. The model fills an urgent need for extensive
waveforms in ongoing data-analysis studies, and its individual components will
continue to be useful in future science-adequate waveforms.
Scientific analysis for the gravitational-wave detector LISA will require
theoretical waveforms from extreme-mass-ratio inspirals (EMRIs) that
extensively cover all possible orbital and spin configurations around
astrophysical Kerr black holes. However, on-the-fly calculations of these
waveforms have not yet overcome the high dimensionality of the parameter space.
To confront this challenge, we present a user-ready EMRI waveform model for
generic (eccentric and inclined) orbits in Kerr spacetime, using an analytical
self-force approach. Our model accurately covers all EMRIs with arbitrary
inclination and black hole spin, up to modest eccentricity ($lesssim 0.3$) and
separation ($gtrsim2$–$10M$ from the last stable orbit). In that regime, our
waveforms are accurate at the leading `adiabatic’ order, and they approximately
capture transient self-force resonances that significantly impact the
gravitational-wave phase. The model fills an urgent need for extensive
waveforms in ongoing data-analysis studies, and its individual components will
continue to be useful in future science-adequate waveforms.
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