REVIEW 35 cited by
Constraints on a phenomenologically parameterized neutron-star equation of state
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
Signed reviews
read the original abstract
We introduce a parameterized high-density equation of state (EOS) in order to systematize the study of constraints placed by astrophysical observations on the nature of neutron-star matter. To obtain useful constraints, the number of parameters should be smaller than the number of neutron-star properties that have been measured or will have been measured in the next several years. And the set must be large enough to accurately approximate the large set of candidate EOSs. We find that a parameterized EOS based on piecewise polytropes with 3 free parameters matches to about 4% rms error an extensive set of candidate EOSs at densities below the central density of 1.4 solar mass stars. Adding observations of more massive stars constrains the higher density part of the EOS and requires an additional parameter. We obtain constraints on the allowed parameter space set by causality and by present and near-future astronomical observations. In particular, we emphasize potentially stringent constraints on the EOS parameter space associated with two measured properties of a single star; and we find that a measurement of the moment of inertia of PSR J0737-3039A can strongly constrain the maximum neutron-star mass. We also present in an appendix a more efficient algorithm than has previously been used for finding points of marginal stability and the maximum angular velocity of stable stars.
Forward citations
Cited by 35 Pith papers
-
From Multimessenger Inference to Simulations: A Ranked Ensemble of Finite-Temperature Equations of State
The paper constructs a 12-member ensemble of finite-temperature neutron star equations of state that spans the posterior from multimessenger and nuclear-physics constraints and releases simulation-ready tables.
-
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.
-
Systematic study of the morphology and length of slow stable hybrid star branches
Systematic numerical survey classifies four types of slow stable hybrid star branches and shows slow conversion opens new viable parameter space for stiff hadronic models.
-
Detection of relativistic orbital deformation from improved timing of PSR J1757$-$1854
First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.
-
The Non-parametric Equation of State Realizes a Generalized Quark-Hadron Crossover
Non-parametric EOS construction shows non-conformal behavior with evidence for soft quark matter and a hadron-quark phase transition in massive neutron star cores.
-
Strongly Interacting Dark Matter admixed Neutron Stars
Strongly interacting dark matter described by a first-principles G2 gauge-theory equation of state can be mixed into neutron stars while remaining compatible with current observational constraints.
-
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.
-
Measuring the electric dipole moment of the neutron using neutron star spin-down
The thesis derives a conditional 90% limit |d_n| < 4.42e-25 e cm from the spin-down budget of PSR J0437-4715 via an effective magnetic-quadrupole channel, the first astrophysical bound of this kind.
-
GRACE: An Open-Source Framework for GPU-Accelerated Numerical Relativity
GRACE is a validated, open-source, Kokkos+p4est GPU-portable framework that evolves ideal GRMHD with constrained transport self-consistently coupled to Z4c Einstein equations on fixed or adaptive meshes.
-
Establishing Compactness as a Population Observable in Gravitational-Wave Astronomy
Hierarchical analysis of GWTC-3 yields C_eff = 0.5^{+0.3}_{-0.1} consistent with black holes and limits low-compactness exotic binary merger rate to <0.7 Gpc^{-3} yr^{-1}.
-
Radial Oscillations of Viscous Stars at Finite Temperature
Heat diffusion introduces a distinct thermal mode sector in viscous star oscillations that transitions to propagating behavior above a critical overtone, realizing finite-size relativistic second sound.
-
Donutization Inside Neutron Stars: Shell-Localized Scalar Fields
Heavy scalar fields in neutron stars form interior shell-localized profiles that reshape the effective equation of state and break the I-Q relation while remaining hidden from binary pulsar observations.
-
Combining simulation-based inference and universal relations for precise and accurate neutron star science
A machine-learning simulator trained on 1,491 simulated equations of state discovers a neutron-star radius relation R(M,f,p1), predicting radii to tens of meters with calibrated error bars.
-
Universal Relations with Dynamical Tides
New quasi-universal relations connect static tidal deformability Λ⁰ to its dynamical correction Λ² and to Mω* with equation-of-state scatter below 5% and 2.8% respectively across 59 models.
-
Remnant properties of binary neutron star mergers undergoing prompt collapse
Prompt-collapse neutron star merger remnants occupy a narrow, high-spin region of the mass-spin plane, and Cosmic Explorer could use tidal deformability to classify most such mergers as neutron star events out to 100-250 Mpc.
-
Distinguishing Neutron Star vs. Low-Mass Black Hole Binaries with Late Inspiral & Postmerger Gravitational Waves $-$ Sensitivity to Transmuted Black Holes and Non-Annihilating Dark Matter
Future high-frequency-sensitive GW detectors can distinguish binary neutron star from low-mass black hole mergers in late phases, enabling separation of merger rates and constraints on heavy non-annihilating dark matt...
-
Systematics from NICER Pulse Profiles Drive Uncertainty in Multi-Messenger Inference of the Neutron Star Equation of State
A joint Bayesian analysis of NICER, gravitational wave, radio, and nuclear data shows that NICER pulse profile modeling choices dominate equation of state uncertainties and prefer the ST+PDT model over the PDT-U model...
-
Black-hole - neutron-star mergers: new numerical-relativity simulations and multipolar effective-one-body model with spin precession and eccentricity
A new catalog of 52 numerical-relativity BHNS merger simulations is used to calibrate TEOBResumS-Dalí, an improved effective-one-body waveform model with multipolar ringdown, spin precession, and eccentricity.
-
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.
-
SACRA-2D: New axisymmetric general relativistic hydrodynamics code with fixed mesh refinement
SACRA-2D is a new axisymmetric relativistic hydrodynamics code with the HLLC solver and adaptive mesh refinement, validated by benchmarks showing improved accuracy over the TVDLF solver.
-
Braneworld Neutron Stars: Constraining Brane Tension with Observational Data
Using six neutron star equations of state, braneworld gravity can support the 2.5 to 2.67 solar mass object seen in GW190814 and gives a lower bound on brane tension near 2×10^37 dyne/cm^2.
-
Tidal effects in gravitational waves from neutron stars in scalar-tensor theories of gravity
Tidal contributions to neutron-star binary gravitational-wave phase in scalar-tensor gravity involve scalar, tensor, and mixed Love numbers, and generally combine to reduce the net tidal signal below the general-relat...
-
Decoding Long-duration Gravitational Waves from Binary Neutron Stars with Machine Learning: Parameter Estimation and Equations of State
Normalizing flows with multibanding, heterodyning, and neural compression can produce BNS parameter posteriors and EOS constraints for 3G-detector signals in about a second, with accuracy restored by importance sampling.
-
Cooling binary neutron star remnants via nucleon-nucleon-axion bremsstrahlung
Nucleon-nucleon-axion bremsstrahlung cooling in binary neutron star merger remnants is too weak to leave a detectable imprint on gravitational waves or ejecta, so it cannot improve axion mass constraints.
-
Inferring prompt black-hole formation in neutron star mergers from gravitational-wave data
Two gravitational-wave inference methods, based on the merger mass threshold and the tidal deformability threshold, estimate a 50-70% prompt black-hole formation probability for GW170817, falling below 10% when pulsar...
-
Smooth equations of state for high-accuracy simulations of neutron star binaries
Spectral equations of state reduce cost and improve accuracy in SpEC neutron star merger simulations, but the most efficient choice requires an unrealistic low-density recipe.
-
Simulating Binary Neutron Stars with Hybrid Equation of States: Gravitational Waves, Electromagnetic Signatures, and Challenges for Numerical Relativity
Numerical relativity simulations of a GW170817-like binary neutron star merger with strange quark matter cores show that strong phase transitions reduce convergence order to first order at insufficient resolution, yet...
-
Extending the infrastructure of the BAM code towards resistive general-relativistic magnetohydrodynamics: tests and first applications
BAM gains a validated resistive GRMHD module; BNS runs show the parallel electric field reaching up to 10% of total strength in low-density disks, unlike ideal MHD.
-
Reconciling GW170817 and GW190814 with a Nonmonotonic Sound-Speed Equation of State
A constrained evolutionary pipeline identifies over 14,000 causal EoS reconciling GW170817 and GW190814 with non-monotonic sound speeds, M_max 2.3-2.8 solar masses, and R_1.4 around 12 km.
-
PSR J0952-0607: Probing the Stiffest Equations of State and r-Mode Suppression Mechanisms
Using the 709.2 Hz spin of PSR J0952-0607 in Bayesian equation-of-state inference shifts its inferred non-rotating mass to 2.10+0.25-0.24 Msun and makes r-mode stability depend on crust rigidity.
-
Bayesian analysis of the shear modulus in the neutron-star crust
Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.
-
Equation of State Extrapolation Systematics: Parametric vs. Nonparametric Inference of Neutron Star Structure
Nonparametric GP-based high-density extensions yield softer EOS posteriors with larger uncertainties than parametric PP extensions when jointly constrained by multi-messenger neutron star observations.
-
Topological Uncertainty for Anomaly Detection in the Neural-network EoS Inference with Neutron Star Data
Applying Topological Uncertainty to hidden-layer activations of a trained FNN detects failed neutron-star EoS inferences with over 90% success in the best-tested configuration.
-
Probing Neutron Star Interiors and the Properties of Cold Ultra-dense Matter with the SKAO
SKAO's sensitivity, surveys and sub-arraying will deliver tighter NS mass, MoI, spin, glitch and precession constraints that, with X-ray and GW data, probe cold ultra-dense matter.
-
Fast and Accurate Prediction of Neutron Star Structure with Deep Neural Networks
Feedforward and residual neural networks predict neutron star observables from piecewise polytropic EOS parameters with R^2>0.999 and a ~200x speedup over direct TOV integration.
Discussion (0). Continue with ORCID to comment.