REVIEW 8 cited by
Schott term in the binding energy for compact binaries on circular orbits at fourth post-Newtonian 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
Schott term in the binding energy for compact binaries on circular orbits at fourth post-Newtonian order
read the original abstract
The phasing for compact binary systems on circular orbits was obtained in arXiv:2304.11185 at fourth-and-a-half post-Newtonian (4.5PN) order thanks to two main ingredients: the 4PN conservative energy (associated to a nonradiative spacetime) in terms of the orbital frequency and the 4.5PN flux in terms of the waveform frequency (i.e., the half-frequency of the $(\ell,m)=(2,2)$ mode). When obtaining the phasing, a key physical postulate was made: the expression of the binding energy in terms of the waveform frequency was assumed to be identical to the expression of the conservative energy in terms of the orbital frequency. This postulate was necessary to ensure that the frequency evolution obtained through the flux-balance law (which involves the binding energy) was independent of the choice of spacetime foliation. In this work, I show that the binding energy entering the flux-balance law differs from the 4PN conservative energy by a 4PN pseudo-Schott term, associated with radiation-reaction effects due to gravitational tails. Unlike the usual Schott terms (at 2.5PN, 3.5PN and 4.5PN), the pseudo-Schott term is not a total derivative and is in fact hereditary, so it does not vanish for circular orbits. Remarkably, the binding energy thus obtained is in perfect agreement with the one obtained using the aforementioned physical postulate, which confirms that the 4.5PN phasing associated to the waveform frequency computed in arXiv:2304.11185 is indeed correct. This result is extended to the other Poincar\'e invariants, and `thermodynamic' relations between the binding energy and angular momentum are established. Finally, the chirp and phasing associated to the orbital frequency are presented at 4.5PN, including horizon-absorption effects.
Forward citations
Cited by 8 Pith papers
-
Constants of motion and fundamental frequencies for elliptic orbits at fourth post-Newtonian order
Derives the 4PN conservative map between constants of motion and fundamental frequencies for eccentric orbits, resummed over eccentricity and validated against circular-orbit and self-force results.
-
Quadrupole and quadratic-in-spin effects in quasicircular, spinning, asymmetric binaries
Calculates energy fluxes with quadratic-in-spin and quadrupole effects for small-mass-ratio spinning binaries in self-force theory, providing numerical data and sixth-order PN expansions.
-
Gravitational radiation reaction for compact binary systems at the fourth-and-a-half post-Newtonian order in harmonic coordinates
The 4.5PN radiation-reaction acceleration of nonspinning compact binaries is derived in harmonic coordinates, including a dimensional-regularization pole, and is shown to satisfy flux-balance laws and Lorentz invariance.
-
Convergence of post-Newtonian for quasi-circular non-precessing comparable mass ratios BBHs
For orbital velocities below 0.45, PN energy flux agreement with NR improves up to incomplete 6PN with non-monotonic behavior, but convergence is lost near v approximately 0.5.
-
Conservative and dissipative sectors in a nonlinear scalar model for the gravitational self-force problem
Multiple Hamiltonian definitions of the conservative second-order self-force are identified in a nonlinear scalar toy model, restricted to unbound scattering trajectories.
-
Fixing the center-of-mass frame of numerical relativity waveforms using the post-Newtonian center-of-mass charge
A post-Newtonian boosted center-of-mass charge template makes numerical-relativity frame-fixing up to ~25x more robust to the fitting-window choice.
-
Fixing the center-of-mass frame of numerical relativity waveforms using the post-Newtonian center-of-mass charge
A post-Newtonian model of the boosted center-of-mass charge makes BMS frame-fixing of nonprecessing, unequal-mass NR waveforms less sensitive to the fitting window, reducing parameter variance by up to ~25x.
-
Post-adiabatic self-force waveforms: slowly spinning primary and precessing secondary
Extended 1PA self-force waveforms for slowly spinning primary and precessing secondary, with re-summed 1PAT1R variant showing improved accuracy against NR for q ≳ 5 and |χ1| ≲ 0.1.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.