REVIEW 5 cited by
Spin contributions to the gravitational-waveform modes for spin-aligned binaries at the 3.5PN order
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
read the original abstract
We complete the post-Newtonian (PN) prediction at the 3.5PN order for the spin contributions to the gravitational waveforms emitted by inspiraling compact binaries, in the case of quasi-circular, equatorial orbits, where both spins are aligned with the orbital angular momentum. Using results from the multipolar post-Minkowskian wave generation formalism, we extend previous works that derived the dynamics and gravitational-wave energy flux and phasing, by computing the full waveform decomposed in spin-weighted spherical harmonics. This new calculation requires the computation of multipolar moments of higher multipolar order, new quadratic-in-spin contributions to the hereditary tail terms entering at the 3.5PN order, as well as other non-linear interactions between moments. When specialized to the test-mass limit, our results are equivalent to those obtained in the literature for the waveform emitted by a test-mass in equatorial, circular orbits around a Kerr black hole. We also compute the factorized modes for use in effective-one-body waveform models, correcting the 2.5PN nonspinning and 3PN quadratic-in-spin terms in the (2,1) mode used in current models.
Forward citations
Cited by 5 Pith papers
-
Tidal contributions to the full gravitational waveform to the second-and-a-half post-Newtonian order
Tidal contributions to all gravitational waveform amplitude modes up to l=7 are derived to 2.5PN for quasi-circular non-spinning compact binaries, with flux and phasing provided at the same order.
-
Third post-Newtonian dynamics for eccentric orbits and aligned spins in the effective-one-body waveform model SEOBNRv5EHM
The authors obtain, for the first time, 3PN-accurate eccentric-orbit fluxes, radiation-reaction force, and waveform modes in the effective-one-body formalism, and use them to build the SEOBNRv5EHM inspiral model.
-
Advancing the Effective-One-Body Framework in the Test-Mass Limit
SEOB-TML cuts dephasing by up to an order of magnitude in the test-mass limit by Q-factorizing the flux (including horizon absorption) and by modeling mode mixing with extracted QNM coefficients.
-
Early Warning From Eccentric Compact Binaries: Template Initialization And Sub-dominant Mode Effects
For eccentric neutron star and black hole binaries, initializing early-warning templates at the periastron frequency, and including subdominant waveform modes, measurably improves sky localization and early warning time.
-
Spin effects in the phasing formula of eccentric compact binary inspirals up to the third post-Newtonian order
Closed-form post-Newtonian phasing formulas for eccentric, spin-aligned compact binary inspirals are derived to 3PN order and to eighth order in initial eccentricity, with a resummation extending validity to e0 around 0.55.
Discussion (0). Continue with ORCID to comment.