Constraining neutron-star tidal Love numbers with gravitational-wave detectors

By E. Flanagan, T. Hinderer. 2007

743 citations recorded by the source corpus.

Ground-based gravitational wave detectors may be able to constrain the nuclear equation of state using the early, low frequency portion of the signal of detected neutron star--neutron star inspirals. In this early adiabatic regime, the influence of a neutron star's internal structure on the phase of the waveform depends only on a single parameter $\ensuremath{\lambda}$ of the star related to its tidal Love number, namely, the ratio of the induced quadrupole moment to the perturbing tidal gravitational field. We analyze the information obtainable from gravitational wave frequencies smaller than a cutoff frequency of 400 Hz, where corrections to the internal-structure signal are less than 10%. For an inspiral of two nonspinning $1.4{M}_{\ensuremath{\bigodot}}$ neutron stars at a distance of 50 Megaparsecs, LIGO II detectors will be able to constrain $\ensuremath{\lambda}$ to $\ensuremath{\lambda}\ensuremath{\le}2.0\ifmmode\times\else\texttimes\fi{}{10}^{37}\text{ }\text{ }\mathrm{g}\text{ }{\mathrm{cm}}^{2}\text{ }{\mathrm{s}}^{2}$ with 90% confidence. Fully relativistic stellar models show that the corresponding constraint on radius $R$ for $1.4{M}_{\ensuremath{\bigodot}}$ neutron stars would be $R\ensuremath{\le}13.6\text{ }\text{ }\mathrm{km}$ (15.3 km) for a $n=0.5$ ($n=1.0$) polytrope with equation of state $p\ensuremath{\propto}{\ensuremath{\rho}}^{1+1/n}$.

Subfields: Astronomy and Astrophysics, Geophysics, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/d62fe4aa10a9811b8795834dcea09b36b22de79f

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 Ocean Engineering

Citations in the corpus

Mass Ejection from the Remnant of a Binary Neutron Star Merger: Viscous-radiation Hydrodynamics Study (2017, background): “The tidal deformability together with the mass will give us invaluable information for exploring the properties of the high-density nuclear matter (Flanagan & Hinderer 2008).”
Stellar structure models in modified theories of gravity: Lessons and challenges (2019, background): “13km (90% confidence level), which in turns allows to rule out sufficiently soft EOS in the context of GR [397], as well as to obtain the information encoded in the change of the gravitational wave phase caused by the tidal deformability exerted by each neutron star [398].”
Tidal Deformability from GW170817 as a Direct Probe of the Neutron Star Radius (2018, methodology): “Nevertheless, Flanagan & Hinderer (2008) found that the early phase of the inspiral depends cleanly on a single EOS-dependent parameter: the tidal Love number, λ.”
GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations (2017, background): “LIGO and Virgo observations also constrain tidal effects in the inspiral by placing an upper bound on the dimensionless quantity (Flanagan & Hinderer 2008; Favata 2014) M M M M M A B 16 13 12 , 1A B A A A B 4 5 L = + L + + « ⎡ ⎣⎢ ⎤ ⎦⎥ ˜ ( ) ˜ ( ) ( ) ( ) which is inferred to be smaller than 800 at…”
Dark halos around neutron stars and gravitational waves (2018, background): “is the relevant measure of the tidal deformability of the BNS system [34].”
Tidal Love Numbers of Neutron Stars (2007, methodology): “Flanagan & Hinderer (2008) have shown that for an inspiral of two nonspinning 1:4 M NSs at a distance of 50 Mpc, LIGO II detectors will be able to constrain k to k 2:01 ; 1037 g cm2 s2 with 90% confidence.”
Black hole perturbation theory and gravitational self-force (2021, neutral): “15 These calculations represent one of the major applications of the methods of black hole perturbation theory reviewed in the previous section, and they form part of an ongoing endeavour to include tidal effects in gravitational-wave templates and to infer properties of neutron stars from observed ”
Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis (2018, background): “Figure 6 shows ejecta masses and velocities as a function of the tidal deformability of the binary L̃ (e.g., Flanagan & Hinderer 2008; Favata 2014).”
The tune of love and the nature(ness) of spacetime (2016, methodology): “The Love number may be then obtained from the GW phase [44]8”
Properties of the Binary Neutron Star Merger GW170817 (2018, background): “In the post-Newtonian formalism, matter effects for nonspinning objects first enter the waveform phase at 5PN order through the tidally induced quadrupolar (l 1⁄4 2) deformation [135].”