Tidal Love numbers of neutron and self-bound quark stars

By S. Postnikov, M. Prakash, J. Lattimer. 2010

243 citations recorded by the source corpus.

Gravitational waves from the final stages of inspiraling binary neutron stars are expected to be one of the most important sources for ground-based gravitational wave detectors. The masses of the components are determinable from the orbital and chirp frequencies during the early part of the evolution, and large finite-size (tidal) effects are measurable toward the end of inspiral, but the gravitational wave signal is expected to be very complex at this time. Tidal effects during the early part of the evolution will form a very small correction, but during this phase the signal is relatively clean. The accumulated phase shift due to tidal corrections is characterized by a single quantity related to a star's tidal Love number. The Love number is sensitive, in particular, to the compactness parameter M/R and the star's internal structure, and its determination could provide an important constraint to the neutron star radius. We show that Love numbers of self-bound strange quark matter stars are qualitatively different from those of normal neutron stars. Observations of the tidal signature from coalescing compact binaries could therefore provide an important, and possibly unique, way to distinguish self-bound strange quark stars from normal neutron stars. Tidal signatures from self-bound strangemore » quark stars with masses smaller than 1M{sub {center_dot}}are substantially smaller than those of normal stars owing to their smaller radii. Thus tidal signatures of stars less massive than 1M{sub {center_dot}}are probably not detectable with Advanced LIGO. For stars with masses in the range 1-2M{sub {center_dot},} the anticipated efficiency of the proposed Einstein telescope would be required for the detection of tidal signatures.« less

Subfields: Astronomy and Astrophysics, Geophysics, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/72dde889a4696cf7f6b924dfd76686846526f5c7

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Citations in the corpus

Multi-resonance orbital model of high-frequency quasi-periodic oscillations: possible high-precision determination of black hole and neutron star spin (2013, background): “It is well known that the neutron star mass surely cannot exceed the critical value ofM ∼ 3 M⊙ (Rhoades & Ruffini 1974) and the models based on the realistic equations of state give maximal masses going up toMmax ∼ 2.8 M⊙ (Postnikov et al. 2010).”
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).”