Calculating the scalar self-force experienced by extreme-mass-ratio binaries during rθ-resonances

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Calculatingthescalarselfforceexperiencedbyextrememassratio.pdf (3.28 MB)

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https://meetings.aps.org/Meeting/APR20/Session/T16.2

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http://hdl.handle.net/11603/40032

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UMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)

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Author/Creator ORCID

https://orcid.org/0000-0002-5109-9704

Date

2020-04-20

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presentations (communicative events)
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Citation of Original Publication

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This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Abstract

A vast majority of extreme-mass-ratio black hole binaries (EMRIs) will encounter at least one strong rθ-resonance as they evolve through LISA's passband. These resonances occur when the frequencies of the librating radial and polar motion of the EMRI's smaller body form a low-integer ratio, and they drive significant `kicks' in the amount of energy and angular momentum that EMRIs radiate through gravitational waves. These kicks, if not properly accounted for, can amplify errors in modeled EMRI waveforms by factors of ∼100. Despite the importance of modeling these resonant dynamics, researchers have not yet calculated the gravitational self-force experienced by EMRIs during rθ-resonances. As a first step in quantifying these effects, we calculate the scalar self-force (the scalar analog to the gravitational self-force) experienced by a scalar-charged particle following an rθ-resonant geodesic around a Kerr black hole. We present how local and global radiation-reaction effects vary with respect to initial conditions. We also demonstrate, numerically, that conservative self-force effects do not contribute to the leading-order evolution of the system, as hypothesized by previous researchers.