Tidal deformability of neutron stars with realistic equations of state

By T. Hinderer, B. Lackey, R. Lang, J. Read. 2009

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The early part of the gravitational wave signal of binary neutron-star inspirals can potentially yield robust information on the nuclear equation of state. The influence of a star's internal structure on the waveform is characterized by a single parameter: the tidal deformability $\ensuremath{\lambda}$, which measures the star's quadrupole deformation in response to the companion's perturbing tidal field. We calculate $\ensuremath{\lambda}$ for a wide range of equations of state and find that the value of $\ensuremath{\lambda}$ spans an order of magnitude for the range of equation of state models considered. An analysis of the feasibility of discriminating between neutron-star equations of state with gravitational wave observations of the early part of the inspiral reveals that the measurement error in $\ensuremath{\lambda}$ increases steeply with the total mass of the binary. Comparing the errors with the expected range of $\ensuremath{\lambda}$, we find that Advanced LIGO observations of binaries at a distance of 100 Mpc will probe only unusually stiff equations of state, while the proposed Einstein Telescope is likely to see a clean tidal signature.

Subfields: Astronomy and Astrophysics, Geophysics, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/fac228bec0ac5637839b25f26d390ce0b5098432

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Citations in the corpus

Tidal Deformability from GW170817 as a Direct Probe of the Neutron Star Radius (2018, background): “For realistic, hadronic equations of state, k2 has been constrained to lie in the range ∼ 0.05 − 0.15 (Hinderer 2008; Hinderer et al. 2010; Postnikov et al. 2010).”
GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations (2017, background): “…the NSs is encoded in the phase evolution of the gravitational wave (GW) signal during the inspiral (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…”
Constraining the Maximum Mass of Neutron Stars from Multi-messenger Observations of GW170817 (2017, background): “…of GW detections, such as “standard siren” measurements of the cosmic expansion history (Holz & Hughes 2005; Nissanke et al. 2010; LIGO Scientific Collaboration et al. 2017c) or as probes of the equation of state (EOS) of NSs (e.g. Read et al. 2009; Hinderer et al. 2010; Bauswein & Janka 2012).”
Enhanced sensitivity of the LIGO gravitational wave detector by using squeezed states of light (2013, background): “[28] Hinderer T.”