Adiabatic Waveforms from Extreme-Mass-Ratio Inspirals: An Analytical Approach
Abstract
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 (≲ 0.3) and separation (≳ 2–10 M 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.
Additional Information
© 2022 American Physical Society. (Received 24 November 2021; accepted 6 May 2022; published 10 June 2022) We thank Wataru Hikida and Hideyuki Tagoshi for their direct contributions to an earlier version of this manuscript, Scott A. Hughes for helpful discussions on initial phases and comments on the Supplemental Material, Maarten van de Meent for providing independent numerical data to verify BHPC's Teukolsky results, Leor Barack and Chulmoon Yoo for valuable discussions and comments on the manuscript, and Katsuhiko Ganz, Chris Kavanagh, Koutarou Kyutoku, Yasushi Mino, Takashi Nakamura, Misao Sasaki, Masaru Shibata, and Niels Warburton for very helpful discussions. S. I. is especially grateful to Eric Poisson, Riccardo Sturani, and Takahiro Tanaka for their continuous encouragement and insightful discussion about the (adiabatic) evolution scheme for EMRI dynamics. Finally, we thank all the past and present members of the annual Capra meetings with whom we have discussed the techniques and results presented here (over the past decades). S. I. acknowledges support from STFC through Grant No. ST/R00045X/1, the GWverse COST Action CA16104, "Black holes, gravitational waves and fundamental physic," and the additional financial support of Ministry of Education—MEC during his stay at IIP-Natal-Brazil. A. J. K. C. acknowledges support from the NASA Grants No. 18-LPS18-0027 and 20-LPS20-0005, and from the NSF Grant No. PHY-2011968. A. P. acknowledges the support of a Royal Society University Research Fellowship, Research Grant for Research Fellows, Enhancement Awards, and Exchange Grant. This work was supported in part by JSPS/MEXT KAKENHI Grants No. JP16H02183 (R. F.), JP18H04583 (R. F.), JP21H01082 (R. F., H. N., and N. S.), JP17H06358 (H. N. and N. S.), and JP21K03582 (H. N.).Attached Files
Published - PhysRevLett.128.231101.pdf
Accepted Version - 2111.05288.pdf
Supplemental Material - Supplemental_Material.pdf
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Additional details
- Eprint ID
- 115166
- Resolver ID
- CaltechAUTHORS:20220614-603125000
- ST/R00045X/1
- Science and Technology Facilities Council (STFC)
- CA16104
- European Cooperation in Science and Technology (COST)
- Ministério da Educação
- 18-LPS18-0027
- NASA
- 20-LPS20-0005
- NASA
- PHY-2011968
- NSF
- Royal Society
- JP16H02183
- Japan Society for the Promotion of Science (JSPS)
- JP18H04583
- Japan Society for the Promotion of Science (JSPS)
- JP21H01082
- Japan Society for the Promotion of Science (JSPS)
- JP17H06358
- Japan Society for the Promotion of Science (JSPS)
- JP21K03582
- Japan Society for the Promotion of Science (JSPS)
- Created
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2022-06-15Created from EPrint's datestamp field
- Updated
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2022-06-15Created from EPrint's last_modified field