Post-1-Newtonian tidal effects in the gravitational waveform from binary inspirals

By J. Vines, T. Hinderer, '. Flanagan. 2011

207 citations recorded by the source corpus.

The gravitational wave signal from an inspiralling binary neutron star system will contain detailed information about tidal coupling in the system, and thus, about the internal physics of the neutron stars. To extract this information will require highly accurate models for the gravitational waveform. We present here a calculation of the gravitational wave signal from a binary with quadrupolar tidal interactions which includes all post-1-Newtonian-order effects in both the conservative dynamics and wave generation. We consider stars with adiabatically induced quadrupoles moving in circular orbits, and work to linear order in the stars' quadrupole moments. We find that post-1-Newtonian corrections increase the tidal signal by approximately 20% at gravitational wave frequencies of 400 Hz.

Subfields: Astronomy and Astrophysics, Geophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/5f4e09a7f179d550b9e9f85d6838bdb773c1dc3c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Geophysics

In Oceanography

Citations in the corpus

Tidal Deformability from GW170817 as a Direct Probe of the Neutron Star Radius (2018, methodology): “…with a frequency-domain post-Newtonian waveform model (Sathyaprakash & Dhurandhar 1991), with modifications to account for tidal interactions (Vines et al. 2011), point-mass spin-spin interactions (Mikóczi et al. 2005; Arun et al. 2011; Bohé et al. 2015; Mishra et al. 2016), and effects…”
Unequal mass binary neutron star mergers and multimessenger signals (2016, background): “where k (i) 2 is the quadrupolar tidal coupling Love number constant and Ci = Mi/Ri (for the ith star) [34, 35].”
Enhancing the sensitivity of the LIGO gravitational wave detector by using squeezed states of light (2013, background): “on the poorly understood nuclear equation of state by measurements of the tidal deformability [28, 29], of the post-merger survival time [30], and of mode pulsations of the merged remnant (at frequencies > 2 kHz).”
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 frequencydomain models IMRPhenomPv2NRT [25,26,32,49,99], SEOBNRv4NRT [29,32,77,99], and TaylorF2 [35,36, 38,100–112] and two time-domain models SEOBNRv4T [31] and TEOBResumS [33,113].”
Properties of the Binary Neutron Star Merger GW170817 (2018, unknown): “5PN (PP [60–65], SO [66] SS [67–70]) 6PN [71] None ✗”
Enhanced sensitivity of the LIGO gravitational wave detector by using squeezed states of light (2013, background): “[29] Vines, J.”