Abstract
While most binary inspirals are expected to have circularized before they enter the LIGO/Virgo frequency band, a small fraction of those binaries could have non-negligible orbital eccentricity depending on their formation channel. Hence, it is important to accurately model eccentricity effects in waveform models used to detect those binaries, infer their properties, and shed light on their astrophysical environment. We develop a multipolar effective-one-body (EOB) eccentric waveform model for compact binaries whose components have spins aligned or antialigned with the orbital angular momentum. The waveform model contains eccentricity effects in the radiation-reaction force and gravitational modes through second post-Newtonian (PN) order, including tail effects, and spin-orbit and spin-spin couplings. We recast the PN-expanded, eccentric radiation-reaction force and modes in factorized form so that the newly derived terms can be directly included in the state-of-the-art, quasi-circular--orbit EOB model currently used in LIGO/Virgo analyses (i.e., the SEOBNRv4HM model).
Highlights
The observation of gravitational waves (GWs) by the LIGO-Virgo detectors [1,2] have corroborated the existence of binary black holes (BBHs) in our universe
Extending the waveform models used today in GW astronomy from quasicircular to eccentric orbits is important for future observations with LIGO, Virgo, and KAGRA detectors [21], and with new facilities on the ground (Cosmic Explorer and Einstein Telescope), and in space (LISA)
While this presents a challenge for waveform modeling and data analysis, it offers the unique opportunity to unveil the formation channels of compact binaries and probe their environment
Summary
The observation of gravitational waves (GWs) by the LIGO-Virgo detectors [1,2] have corroborated the existence of binary black holes (BBHs) in our universe. Binaries are expected to circularize [9,10] as they approach merger due to the emission of gravitational radiation Depending on their astrophysical formation channel, a small fraction of binaries could have nonnegligible orbital eccentricity, as they enter the frequency bands of current detectors. [82] added eccentric corrections in the SEOBNRv4 [74,83] waveform model, notably in the (2,2),(2,1),(3,3),(4,4) modes through 2PN order, including spin-orbit (SO) and spin-spin (SS) couplings, but not tail effects. [84,85] incorporated noncircular effects in the TEOBResumS_SM [76,86] model at leading PN order in the azimuthal component of the RR force and used a quasicircular 2PN-expanded radial RR force without spin or tail effects They included eccentric corrections at leading PN order to all modes m ≠ 0 up to l 1⁄4 jmj 1⁄4 5. We provide our results for the RR force and waveform modes as Mathematica files in the Supplemental Material [88]
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