Causality anchored to χEFT at low density implies the closed-form bound R(2.0 M_⊙) ≤ 1.16 R(1.4 M_⊙) − 1.1 km for neutron stars sharing one causal EoS, saturated by an analytic one-parameter family.
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Salmi et al.,The Radius of the High-mass Pulsar PSR J0740+6620 with 3.6 yr of NICER Data,Astrophys
15 Pith papers cite this work. Polarity classification is still indexing.
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Non-parametric EOS construction from crust to pQCD forces a sound-speed peak and softening that realizes a generalized quark-hadron crossover in massive 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.
Multi-wavelength pulse profile modeling of PSR J0437-4715 with radio prior yields mass 1.38±0.03 solar masses and radius 13.25 km at 68% confidence.
An intrinsic degeneracy in two-spot thermal X-ray pulse models creates multi-modal posteriors that can bias neutron star radius estimates by up to 30%.
RGOPT-resummed NNLO pQCD EoS for massive quarks in beta equilibrium is fitted and applied to construct pure quark stars (X=3.08-3.58) and hybrid stars (X~2-2.98) compatible with PSR J0740+6620 and GW190814.
Differential rotation in hybrid stars with deconfinement phase transition allows quasi-toroidal configurations with quark matter rings and leads to degeneracies in rotational profiles at mass-radius curve intersections.
Bayesian analysis finds that the likely ranges of light dark-matter fermion mass and exponential density-profile parameter in hyperon-containing neutron stars are nearly independent of the hadronic model for symmetry-energy slopes between 40 and 58 MeV, with HESS J1731-347 and GW170817 data playing,
A Bayesian combination of eight M-R posteriors for PSR J0030+0451 yields M = 1.46^{+0.09}_{-0.08} M_⊙, R = 12.69^{+0.64}_{-0.55} km while marginalizing over unknown model systematics.
Vector portal fermionic dark matter admixed in neutron stars produces mediator-mass-dependent changes to the equation of state, yielding distinct mass-radius relations and tidal deformabilities that observations can use to constrain the model.
The study examines the effects of hyperons and H-dibaryons on f-mode oscillations in neutron stars using the quark meson coupling model and tests universal relations in the Cowling approximation.
Theoretical inputs and the 2 solar mass lower limit dominate neutron star equation of state constraints across most densities, while radius data refines low densities and higher masses affect wider ranges.
Neutron star observations, especially the heaviest known pulsar masses and GW170817 tidal deformability, provide the strongest restrictions on the allowed cold dense matter equation of state.
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.
Comparative numerical study of radial modes in strange quark stars using CFL, interacting, and linear causal EOS shows all satisfy current mass-radius bounds and produce 4-7 kHz fundamental frequencies.
citing papers explorer
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Causality alone bounds the maximum radius difference between different-mass neutron stars
Causality anchored to χEFT at low density implies the closed-form bound R(2.0 M_⊙) ≤ 1.16 R(1.4 M_⊙) − 1.1 km for neutron stars sharing one causal EoS, saturated by an analytic one-parameter family.
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The Non-parametric Equation of State Realizes a Generalized Quark-Hadron Crossover
Non-parametric EOS construction from crust to pQCD forces a sound-speed peak and softening that realizes a generalized quark-hadron crossover in massive neutron stars.
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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.
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A Hidden Degeneracy in Two-Spot Models for Thermal X-Ray Pulse-Profile Fitting
An intrinsic degeneracy in two-spot thermal X-ray pulse models creates multi-modal posteriors that can bias neutron star radius estimates by up to 30%.
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Quark and hybrid stars with renormalization group improvement of NNLO perturbative QCD
RGOPT-resummed NNLO pQCD EoS for massive quarks in beta equilibrium is fitted and applied to construct pure quark stars (X=3.08-3.58) and hybrid stars (X~2-2.98) compatible with PSR J0740+6620 and GW190814.
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Hybrid Stars with Post-Merger Rotation Profiles
Differential rotation in hybrid stars with deconfinement phase transition allows quasi-toroidal configurations with quark matter rings and leads to degeneracies in rotational profiles at mass-radius curve intersections.
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Bayesian analysis of density profile of light dark matter elucidating the properties of dark matter admixed neutron stars in the presence of hyperons
Bayesian analysis finds that the likely ranges of light dark-matter fermion mass and exponential density-profile parameter in hyperon-containing neutron stars are nearly independent of the hadronic model for symmetry-energy slopes between 40 and 58 MeV, with HESS J1731-347 and GW170817 data playing,
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Combining the Mass--Radius Posteriors of J0030+0451 Allowing for Unknown Model Systematics
A Bayesian combination of eight M-R posteriors for PSR J0030+0451 yields M = 1.46^{+0.09}_{-0.08} M_⊙, R = 12.69^{+0.64}_{-0.55} km while marginalizing over unknown model systematics.
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Neutron star with dark matter using vector portal
Vector portal fermionic dark matter admixed in neutron stars produces mediator-mass-dependent changes to the equation of state, yielding distinct mass-radius relations and tidal deformabilities that observations can use to constrain the model.
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$f$-mode Oscillations for Hyperons and H-dibaryons in Neutron Stars
The study examines the effects of hyperons and H-dibaryons on f-mode oscillations in neutron stars using the quark meson coupling model and tests universal relations in the Cowling approximation.
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Sensitivity of the Neutron Star Equation of State Inferences to Mass and Radius Measurements
Theoretical inputs and the 2 solar mass lower limit dominate neutron star equation of state constraints across most densities, while radius data refines low densities and higher masses affect wider ranges.
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Astrophysical constraints on the cold equation of state of the strongly interacting matter
Neutron star observations, especially the heaviest known pulsar masses and GW170817 tidal deformability, provide the strongest restrictions on the allowed cold dense matter equation of state.
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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.
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Radial oscillations of quark stars in light of current astrophysical constraints: A comparative study
Comparative numerical study of radial modes in strange quark stars using CFL, interacting, and linear causal EOS shows all satisfy current mass-radius bounds and produce 4-7 kHz fundamental frequencies.