REVIEW 14 cited by
Neutron star tidal deformability and equation of state constraints
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Neutron star tidal deformability and equation of state constraints
read the original abstract
Despite their long history and astrophysical importance, some of the key properties of neutron stars are still uncertain. The extreme conditions encountered in their interiors, involving matter of uncertain composition at extreme density and isospin asymmetry, uniquely determine the stars' macroscopic properties within General Relativity. Astrophysical constraints on those macroscopic properties, such as neutron star masses and radii, have long been used to understand the microscopic properties of the matter that forms them. In this article we discuss another astrophysically observable macroscopic property of neutron stars that can be used to study their interiors: their tidal deformation. Neutron stars, much like any other extended object with structure, are tidally deformed when under the influence of an external tidal field. In the context of coalescences of neutron stars observed through their gravitational wave emission, this deformation, quantified through a parameter termed the \emph{tidal deformability}, can be measured. We discuss the role of the tidal deformability in observations of coalescing neutron stars with gravitational waves and how it can be used to probe the internal structure of Nature's most compact matter objects. Perhaps inevitably, a large portion of the discussion will be dictated by GW170817, the most informative confirmed detection of a binary neutron star coalescence with gravitational waves as of the time of writing.
Forward citations
Cited by 14 Pith papers
-
Dynamical Tidal Response of Neutron Stars: from Effective Field Theory to Gravitational Waveforms
Complete leading-order dynamical tidal corrections to neutron-star binaries are derived in EFT, showing dynamical Love numbers enhanced relative to static ones and yielding measurable contributions to the GW phase at ...
-
Dynamical tidal Love numbers of black holes under generic perturbations: Connecting black hole perturbation theory with effective field theory
Dynamical tidal Love numbers for Kerr black holes are obtained to linear frequency order by matching EFT worldline couplings to black-hole perturbation solutions, including spin-induced mode mixing.
-
Axial Oscillations of Viscous Neutron Stars
Viscous neutron stars have new families of axial oscillation modes without perfect-fluid counterparts, featuring mode avoidance and long-lived modes.
-
nmma: An extended Bayesian framework for Nuclear Multimessenger Astronomy in the Era of Next-Generation Detectors
nmma now jointly samples nuclear EoS parameters with GW and EM data via TOV emulators and Fiesta surrogates, delivering 20–60× speedups and future H0–nuclear constraints.
-
Fermionic Love number of higher-dimensional Reissner-Nordstr\"om black holes
Fermionic tidal Love numbers for D-dimensional RN black holes remain nonzero for all angular momentum l (except extremal cases) and lose their l-dependence as D grows to infinity.
-
Axial Oscillations of Viscous Neutron Stars
Causal viscous relativistic hydrodynamics applied to neutron stars yields new axial mode families without perfect-fluid counterparts, including mode avoidance and long-lived modes.
-
Photon counting readout for detection and inference of gravitational waves from neutron star merger remnants
Photon counting readout detects weak postmerger gravitational wave signals at a rate of about 1 in 100 for SNR 0.2 and yields a twofold improvement in neutron star radius measurement after 20,000 events.
-
Inferring neutron-star Love-Q relations from gravitational waves in the hierarchical Bayesian framework
Hierarchical Bayesian inference on 20 high-SNR simulated binary neutron star events shows a linear lnΛ-lnQ relation suffices and constrains dynamical Chern-Simons gravity length scale to ≤10 km.
-
TTE-CAM: Self-Explainable Class Activation Maps for Pretrained Black-Box CNNs
A test-time convolution-head replacement converts pretrained CNNs into self-explainable models that keep black-box accuracy and produce faithful class activation maps.
-
Tracing the Trace Anomaly of Dense Matter inside Neutron Stars
Quasi-universal relations connect the trace anomaly profile of neutron star matter to stellar compactness, moment of inertia, and tidal deformability, yielding a central value estimate of Δ_c = 0.1770^{+0.0365}_{-0.04...
-
Hybrid stars with hyperons: structure based on QCD sum rule coupling constants
Hybrid star EOS constructed from QCDSR couplings in RMF hadronic model and bag/NJL quark models with Gibbs/Maxwell transitions yields mass-radius and tidal deformability predictions.
-
Exploring the Potential for Detecting Rotational Instabilities in Binary Neutron Star Merger Remnants with Gravitational Wave Detectors
Numerical post-merger waveforms indicate that planned 3rd-generation GW detector networks can detect rotational instabilities in BNS remnants at distances up to 200 Mpc with a high-frequency design, and the main post-...
-
Love numbers of black holes and compact objects
A pedagogical review of Love numbers and tidal responses for black holes and compact objects in general relativity and extensions.
-
Inferring the properties of a population of compact binaries in presence of selection effects
Pedagogical derivation from first principles of hierarchical Bayesian inference for population properties of compact binaries in the presence of selection effects, with two worked examples.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.