Adiabatic waveforms from extreme-mass-ratio inspirals: an analytical approach
Adiabatic waveforms from extreme-mass-ratio inspirals: an analytical approach
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.
Isoyama, Soichiro
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Fujita, Ryuichi
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Chua, Alvin
8d55c956-1656-4fdf-8f67-9741105afeda
Nakano, Hiroyuki
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Pound, Adam
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Sago, Norichika
c4baa9a1-e4fb-448e-8818-f7d189ed2773
10 June 2022
Isoyama, Soichiro
b4131dce-d874-4b37-a889-4c4a365f7524
Fujita, Ryuichi
7a3f4571-facf-44a3-94e4-a4fcd4419d5d
Chua, Alvin
8d55c956-1656-4fdf-8f67-9741105afeda
Nakano, Hiroyuki
a11bf0d8-b19e-48f2-a7fa-2da0742c32cc
Pound, Adam
5aac971a-0e07-4383-aff0-a21d43103a70
Sago, Norichika
c4baa9a1-e4fb-448e-8818-f7d189ed2773
Isoyama, Soichiro, Fujita, Ryuichi, Chua, Alvin, Nakano, Hiroyuki, Pound, Adam and Sago, Norichika
(2022)
Adiabatic waveforms from extreme-mass-ratio inspirals: an analytical approach.
Physical Review Letters, 128 (23), [231101].
(doi:10.1103/PhysRevLett.128.231101).
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.
Text
PN_adiabatic
- Accepted Manuscript
More information
Accepted/In Press date: 6 May 2022
e-pub ahead of print date: 10 June 2022
Published date: 10 June 2022
Additional Information:
Funding Information:
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.).
Publisher Copyright:
© 2022 American Physical Society.
Identifiers
Local EPrints ID: 457625
URI: http://eprints.soton.ac.uk/id/eprint/457625
ISSN: 0031-9007
PURE UUID: ff6cde1f-b9c9-41b7-9b55-e35c0d26962b
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Date deposited: 14 Jun 2022 16:45
Last modified: 17 Mar 2024 03:27
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Contributors
Author:
Soichiro Isoyama
Author:
Ryuichi Fujita
Author:
Alvin Chua
Author:
Hiroyuki Nakano
Author:
Norichika Sago
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