Closed-form tidal approximants for binary neutron star gravitational waveforms constructed from high-resolution numerical relativity simulations

By Tim Dietrich, Sebastiano Bernuzzi, Wolfgang Tichy. 2017

169 citations recorded by the source corpus.

We construct closed-form gravitational waveforms (GWs) with tidal effects for the coalescence and merger of binary neutron stars. The method relies on a new set of eccentricity-reduced and high-resolution numerical relativity (NR) simulations and is composed of three steps. First, tidal contributions to the GW phase are extracted from the time-domain NR data. Second, those contributions are employed to fix high-order coefficients in an effective and resummed post-Newtonian expression. Third, frequency-domain tidal approximants are built using the stationary phase approximation. Our tidal approximants are valid from the low frequencies to the strong-field regime and up to merger. They can be analytically added to any binary black hole GW model to obtain a binary neutron star waveform, either in the time or in the frequency domain. This work provides simple, flexible, and accurate models ready to be used in both searches and parameter estimation of binary neutron star events.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/a98b750fcaf46478f89a08fd1660903acb6578fe

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Citations in the corpus

Gravitational waves from neutron star mergers and their relation to the nuclear equation of state (2019, methodology): “ been later noticeably improved by using better numerical-relativity simulations (higher resolutions, smaller initial orbital eccentricity27), better approximants (resummed post-Newtonian expressions [396], tidal eective one body [397]), either in the time domain [396] or directly in the frequency d”
Properties of the Binary Neutron Star Merger GW170817 (2018, methodology): “The other three waveform models begin with point-particle models and add a fit to the phase evolution from tidal effects, labeled NRTidal [74,75], that fit the high-frequency region to both an analytic EOB model [80] and NR simulations [74,89].”
GWTC-2.1: Deep extended catalog of compact binary coalescences observed by LIGO and Virgo during the first half of the third observing run (2021, methodology): “For GW190425, the only O3a event in this catalog classified as a BNS, we follow previous analyses [8, 135], and report findings using the IMRPhenomP NRTidal waveform model [65, 66], which is based upon the BBH model IMRPhenomPv2 [153, 162, 163] with the addition of EoS dependent self-spin effects an”
GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs (2018, methodology): “For the analysis of GW170817 we present results for three frequency-domain models IMRPhenomPv2NRT [24, 25, 31, 48, 92], SEOBNRv4NRT [28, 31, 92, 93], TaylorF2 [34, 35, 37, 94–106] and two time-domain models SEOBNRv4T [30] and TEOBResumS [32, 107].”
GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations (2017, background): “…(Flanagan & Hinderer 2008; Damour & Nagar 2010; Hinderer et al. 2010, 2016; Damour et al. 2012; Del Pozzo et al. 2013; Read et al. 2013; Favata 2014; Wade et al. 2014; Bernuzzi et al. 2015b; Lackey & Wade 2015; Hotokezaka et al. 2016; Lackey et al. 2017; Dietrich et al. 2017a; Kiuchi et al. 2017).”
GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run (2020, methodology): “For the BNS system GW190425 [32], we use the following: IMRPhenomD_NRTidal and IMRPhenomPv2_NRTidal [213,214], which are based on the BBH models IMRPhenomD and IMRPhenomPv2, respectively, and incorporate NR and tidal EOB-tuned contributions from tidal interaction as well as equation-of-state-depende”