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The sum of Love: Exploring the effective tidal deformability of neutron stars
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Finite size effects come into play during the late stages of neutron star binary inspiral, with the tidal deformability of the supranuclear density matter leaving an imprint on the gravitational-wave signal. As demonstrated in the case of GW170817, this leads to a constraint on the neutron star radius (and hence the equation of state). A deeper understanding of the tidal response requires an analysis of both the state and composition of matter. While these aspects may not have dramatic impact, they could lead to systematic effects that need to be kept in mind as the observational data become more precise. As a step in this direction we explore the role of the composition of matter, which is likely to remain "frozen" during the late stages of binary inspiral. We provide the first in-depth analysis of the problem, including estimates of how composition impacts on the effective tidal deformability. The results provide improved insight into how aspects of physics that tend to be "ignored" impact on binary neutron star gravitational-wave signals.
Forward citations
Cited by 5 Pith papers
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A Bound on the Dynamical Love Number
Schwarz–Pick applied to the rescaled retarded tidal response bounds dynamical Love numbers for neutron stars by the static Love number and spectral gap, and constrains black-hole tidal heating.
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Nonlinear hydrodynamics in spinning neutron stars: Theoretical universal relations and equilibrium solutions
Affine-model hydrodynamics shows three-wave NS tidal couplings are fixed by linear Love numbers, yet omit ~1.7 rad of GW phase per star by merger; four-wave terms cannot lock f-modes.
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Effective-one-body model for coalescing binary neutron stars: Incorporating tidal spin and enhanced radiation from dynamical tides
A new EOB model for BNS/NSBH inspirals adds tidal-spin back-reaction and finite-frequency radiation corrections, yielding waveform phase shifts up to a few radians that previous effective Love number models miss.
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Oscillations of Dissipative Neutron Stars: The Impact of Hyperonic Reaction Rates
Finite hyperonic reaction rates, encoded as a complex sound speed, damp neutron-star f-modes and remove hyperonic g-modes before their restoring force vanishes, producing a tidal lag.
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The error budget of binary neutron star merger simulations for configurations with high spin
For highly spinning (chi=0.5) binary neutron stars, evolution code choice is the largest numerical waveform error, and current analytical models disagree with numerical relativity beyond that error after the stars touch.
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