English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

In the adiabatic post-Newtonian (PN) approximation, the phase evolution ofgravitational waves (GWs) from inspiralling compact binaries in quasicircularorbits is computed by equating the change in binding energy with the GW flux.This energy balance equation can be solved in different ways, which result inmultiple approximants of the PN waveforms. Due to the poor convergence of thePN expansion, these approximants tend to differ from each other during the lateinspiral. Which of these approximants should be chosen as templates fordetection and parameter estimation of GWs from inspiraling compact binaries isnot obvious. In this paper, we present estimates of the effective higher order(beyond the currently available 4PN and 3.5PN) non-spinning terms in the PNexpansion of the binding energy and the GW flux that minimize the difference ofmultiple PN approximants (TaylorT1, TaylorT2, TaylorT4, TaylorF2) witheffective one body waveforms calibrated to numerical relativity (EOBNR). Weshow that PN approximants constructed using the effective higher order termsshow significantly better agreement (as compared to 3.5PN) with the inspiralpart of the EOBNR. For non-spinning binaries with component masses $m_{1,2} \in[1.4 M_\odot, 15 M_\odot]$, most of the approximants have a match(faithfulness) of better than 99% with both EOBNR and each other.

Estimating effective higher order terms in the post-Newtonian binding energy and gravitational-wave flux: Non-spinning compact binary inspiral