A unified equation of state of dense matter and neutron star structure

gr-qc 2026-06 unverdicted novelty 8.0 of 10

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 ...

gr-qc 2026-08 conditional novelty 7.0 of 10

Magnetized neutron stars with dipole fields obey a new exact relation between dipole moment and compactness, and approximate EoS-insensitive relations among dipole moment, quadrupole moment, and ellipticity.

gr-qc 2026-07 conditional novelty 7.0 of 10

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.

gr-qc 2026-05 unverdicted novelty 7.0 of 10

In massive Hellings-Nordtvedt theory, a nonzero vector vacuum asymptotically forbids both curvature-vector couplings at once, and the A²R sector yields Schwarzschild-like black holes plus neutron stars that can deviat...

nucl-th 2025-06 conditional novelty 7.0 of 10

A blended meta-model with ab initio-based low-density correction reduces neutron star crust uncertainties and shifts crust-core transition density, pressure, and crustal moment of inertia in Bayesian inference.

gr-qc 2025-01 conditional novelty 7.0 of 10

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.

gr-qc 2023-12 unverdicted novelty 7.0 of 10

Stable neutron-star configurations denser than black holes exist in quasi-topological gravity and may produce detectable gravitational-wave echoes.

astro-ph.HE 2026-07 conditional novelty 6.0 of 10

With ET (and ET+CE), mock multi-messenger BNS catalogues yield ~40–500 EM counterparts per year and, under ideal recovery, constrain R1.4 to ~0.2 km and H0 to ~1 km s−1 Mpc−1.

gr-qc 2026-05 unverdicted novelty 6.0 of 10

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.

gr-qc 2026-05 unverdicted novelty 6.0 of 10

Neutron stars in quasi-topological gravity can be more compact than black holes and radially stable across several equations of state.

gr-qc 2026-02 conditional novelty 6.0 of 10

First numerical evaluation of the exact strong-field post-Newtonian parameters in Brans–Dicke and Entangled Relativity: neutron-star deviations up to ~46% from standard values, and dipolar gravitational-wave predictio...

nucl-th 2026-01 conditional novelty 6.0 of 10

Neutron-star data, run through fast emulators, directly constrain the six two-nucleon low-energy constants of an N2LO chiral Hamiltonian, with future detectors able to strongly pin down the 3P1 channel.

nucl-th 2025-12 conditional novelty 6.0 of 10

In a quasiparticle Fermi liquid with medium-dependent mass, imposing Landau matching makes the bulk viscosity manifestly non-negative and parametrically smaller than shear viscosity at low temperature, ζ/η ∝ (T/μ*)⁴.

gr-qc 2025-07 conditional novelty 6.0 of 10

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.

hep-ph 2025-07 unverdicted novelty 6.0 of 10

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...

astro-ph.HE 2025-07 conditional novelty 6.0 of 10

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...

gr-qc 2025-06 accept novelty 6.0 of 10

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.

nucl-th 2025-05 unverdicted novelty 6.0 of 10

Bayesian NS EoS study using full nuclear posterior distributions and consistent crust modeling finds increased surface thickness and crustal moment of inertia relative to prior work.

nucl-th 2025-01 conditional novelty 6.0 of 10

A Bayesian framework with analytical TOV linear-response gradients and a neural-network equation of state reconstructs neutron star EoSs and constrains first-order phase transition parameters from simulated mass-radius data.

gr-qc 2025-01 conditional novelty 6.0 of 10

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.

nucl-th 2024-12 reject novelty 6.0 of 10

The paper expresses the bulk and shear viscosities of cold dense nucleon matter through derivatives of the thermodynamic potential, and claims that the positivity of bulk viscosity imposes an independent stability con...

gr-qc 2019-09 accept novelty 6.0 of 10

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.

astro-ph.HE 2019-08 conditional novelty 6.0 of 10

Hybrid SLy plus holographic V-QCD equations of state shift neutron-star merger post-merger gravitational wave peaks to lower frequencies, with f3 most visible near 1.4 solar masses.

gr-qc 2019-08 conditional novelty 6.0 of 10

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...

astro-ph.HE 2026-08 conditional novelty 5.0 of 10

A Bayesian analysis of smooth hadron-quark crossover neutron stars using NICER and GW170817 data favors a broad, high-density mixed transition, disfavors pure quark cores, and makes a neutron-star interpretation of GW...

nucl-th 2026-08 conditional novelty 5.0 of 10

A unified relativistic mean-field model connects white dwarfs to neutron stars and finds light-element seeds shift neutron star radii by roughly 0.2 km at 1.4 solar masses.

gr-qc 2026-08 reject novelty 5.0 of 10

A two-fluid Tolman-Oppenheimer-Volkoff calculation with Einasto dark matter halos produces static solutions where g_rr^{-1} turns negative in a shell outside the neutron star, which the authors call a neutron star ins...

astro-ph.HE 2026-07 conditional novelty 5.0 of 10

The slope of the high-density sound-speed curve shifts the post-merger gravitational-wave peak frequency and ejecta mass, and that peak frequency partially correlates with an integrated 'intrinsic tidal response' — bu...

astro-ph.HE 2026-07 conditional novelty 5.0 of 10

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.

astro-ph.HE 2026-07 conditional novelty 5.0 of 10

Future CE+ET detectors may detect lensed BNS kilonovae at ~0.5/yr via pointed follow-up of known galaxy lenses, while lensed sGRBs and afterglows remain rare or undetectable with current-generation facilities.

gr-qc 2026-06 unverdicted novelty 5.0 of 10

Dark matter admixed neutron stars show up to 12% thinner crusts and higher torsional oscillation frequencies than pure neutron stars when dark matter forms a core, with analytical formulas matching numerics at sub-per...

astro-ph.HE 2026-05 unverdicted novelty 5.0 of 10

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.

astro-ph.HE 2025-11 unverdicted novelty 5.0 of 10

A small vacuum-like dark-energy admixture in neutron stars with 400 MeV–1 GeV fermionic dark matter shrinks halo-induced radius differences from several kilometers to sub-kilometer scales and mass differences to ≲1%.

gr-qc 2025-10 unverdicted novelty 5.0 of 10

Simulations of ET and CE networks show delays degrade localization metrics far more than SNR, with LIGO India greatly reducing the impact for multi-messenger and stochastic searches.

gr-qc 2025-09 conditional novelty 5.0 of 10

Solving modified Tolman-Oppenheimer-Volkoff equations with Bardeen and Hayward nonlinear electrodynamics, this paper finds that neutron stars reach 'frozen states' with a critical horizon at a critical magnetic charge.

astro-ph.HE 2025-02 conditional novelty 5.0 of 10

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.

gr-qc 2019-09 conditional novelty 5.0 of 10

A mock-data study projects that forty binary neutron star detections, dominated by the eight loudest events, will constrain the 1.4-solar-mass neutron star radius to about 10% and the pressure at twice nuclear saturat...

astro-ph.HE 2019-08 conditional novelty 5.0 of 10

Up-down quark stars in the two-families scenario yield tidal deformabilities compatible with GW170817, constraining the effective bag constant to approximately 50 MeV/fm^3.

gr-qc 2026-07 conditional novelty 4.0 of 10

A large-tension braneworld with α_U ≈ −0.15 fits NICER and GW170817 data for SLy, raising M_max to ~2.30 M_⊙ and R_1.4 to ~13.3 km relative to GR.

astro-ph.HE 2026-06 unverdicted novelty 4.0 of 10

Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.

nucl-th 2026-06 unverdicted novelty 4.0 of 10

Higher-order isospin corrections in Skyrme EOSs significantly modify composition-sensitive quantities like proton fraction and chemical potential difference at supra-nuclear densities but leave bulk thermodynamic prop...

astro-ph.IM 2026-06 unverdicted novelty 4.0 of 10

PyCBC Live for O4 adds time-dependent background modeling, early warning search, and improved autogating, delivering sensitivity gains of 1.7-2.3x for coincident searches in mock data challenges.

astro-ph.HE 2026-05 unverdicted novelty 4.0 of 10

Simulations show the low-T/|W| instability develops robustly across five nuclear EOS in a rapidly rotating 35 M⊙ progenitor, with dominant GW frequency correlating to PNS compactness and stiffness.

gr-qc 2026-05 unverdicted novelty 4.0 of 10

Axial w-mode frequencies of anisotropic neutron stars decrease monotonically with mass, depend approximately linearly on compactness with anisotropy modifying slope and intercept, damping times increase with mass, and...

gr-qc 2025-12 unverdicted novelty 4.0 of 10

Moderate positive pressure anisotropy raises neutron star maximum mass to about 2.4 solar masses and compactness by up to 20 percent, with curvature scalars tied to matter showing strong sensitivity while the Weyl sca...

astro-ph.HE 2025-09 unverdicted novelty 4.0 of 10

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.

gr-qc 2025-07 conditional novelty 4.0 of 10

Using four vector f(R) gravity inflation models and nine equations of state, the TOV solver finds that the MPA1 equation of state yields neutron star maximum masses around 2.75 solar masses, inside the mass gap.

astro-ph.HE 2025-06 accept novelty 4.0 of 10

CUTER v2 reconstructs the missing or inconsistent low-density crust of arbitrary neutron-star equations of state, producing unified EoSs whose global properties match original models to within about one percent.

astro-ph.HE 2026-07 accept novelty 3.5 of 10

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.