Hybrid stars containing the 2SC+<dd> phase cool more slowly than those with the 2SC phase because inherited 3P2 superfluidity suppresses quark beta decay, producing cooling curves close to the CFL case.
hub Canonical reference
A Massive Pulsar in a Compact Relativistic Binary
Canonical reference. 100% of citing Pith papers cite this work as background.
34
Pith papers citing it
Background
100% of classified citations
abstract
Many physically motivated extensions to general relativity (GR) predict significant deviations in the properties of spacetime surrounding massive neutron stars. We report the measurement of a 2.01 +/- 0.04 solar mass pulsar in a 2.46-hr orbit with a 0.172 +/- 0.003 solar mass white dwarf. The high pulsar mass and the compact orbit make this system a sensitive laboratory of a previously untested strong-field gravity regime. Thus far, the observed orbital decay agrees with GR, supporting its validity even for the extreme conditions present in the system. The resulting constraints on deviations support the use of GR-based templates for ground-based gravitational wave detectors. Additionally, the system strengthens recent constraints on the properties of dense matter and provides insight to binary stellar astrophysics and pulsar recycling.
hub tools
citation-role summary
background 8
citation-polarity summary
roles
background 8polarities
background 8representative citing papers
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.
Field equation analysis near infinity in massive Hellings-Nordtvedt theory restricts the model to two single-coupling sectors; the A²R sector yields asymptotically flat Schwarzschild black holes with radial vector fields and neutron stars with measurable deviations from GR while satisfying weak-fiel
Bayesian analysis of a smooth hadron-quark crossover EOS finds current observations tightly constrain the density dependence of nuclear symmetry energy while leaving highest-density hadronic and quark-matter parameters only weakly constrained.
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.
Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.
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.
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.
A conservative f(R,T) gravity reformulation decouples the gravitational sector from the microphysical equation of state, enabling computation of neutron star mass-radius relations and tidal deformabilities that satisfy current astrophysical constraints.
A physics-informed Bayesian neural network learns neutron-star equations of state from theoretical priors and constraints, then generates posterior mass-radius and mass-tidal-deformability distributions consistent with NICER radii and 2-solar-mass limits.
Emulator-assisted Bayesian inference of an extended Skyrme EDF, jointly constrained by nuclear observables, ab initio calculations, and NICER data, produces posteriors yielding consistent neutron star crust and core properties with a provided multivariate Gaussian for bulk nuclear matter parameters.
Joint NICER+IXPE pulse-profile modeling of SRGA J144459.2-604207 favors large neutron-star mass and radius with two independent hotspots but shows strong sensitivity to joint-analysis methodology.
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.
Axial modes of anisotropic neutron stars are integrated numerically for realistic EOS; frequency falls with mass, damping time rises, and scaled quantities follow a near-universal quadratic in compactness that is largely EOS-insensitive but mildly model-dependent.
Roughly half of realistic neutron-star equations of state produce stars with negative Ricci scalar inside, and an improved analytic fit links gravitational mass M to baryonic mass Mb with maximum 3 percent variance.
Holographic model of massive deconfined quarks yields a stiff enough equation of state to allow stable 2-solar-mass hybrid stars with quark cores for certain nuclear phases.
Different parametrizations of density dependence in covariant density functionals produce significant variations in the high-density equation of state and symmetry energy, with rational-function forms providing flexibility when saturation properties are adjusted and constrained by multimessenger ast
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}_{-0.0432} for a 1.4 M_⊙ star.
Analytical expressions for ALP-photon conversion in transient compact stars yield an updated bound g_aγ < 5×10^{-12} GeV^{-1} for m_a ≲ 10^{-9} eV from SN 1987A, plus sensitivity forecasts for future Galactic SN and NSM observations.
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.
Dynamical friction from a degenerate fermionic dark matter background induces measurable secular decay in binary pulsar orbital periods, with sensitivity to fermion masses ≳50 eV and example upper bounds around 1 keV from Milky Way data.
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.
Bayesian modeling with informed priors reduces uncertainties in neutron-star crust shear properties, predicting torsional mode frequencies of 20-50 Hz compatible with observations.
Bayesian analysis of generic hybrid EOS with first-order deconfinement shows mass-gap hybrids require early transition and stiff quark matter, but data favor twins at 1.4 M_sun that exclude them.
citing papers explorer
-
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.
-
Massquerade: Impacts of Mass Ratio Reversals on Binary Black Hole Merger Rates and Mass Distributions
Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.
-
A Physics Informed Bayesian Neural Network for the Neutron Star Equation of State
A physics-informed Bayesian neural network learns neutron-star equations of state from theoretical priors and constraints, then generates posterior mass-radius and mass-tidal-deformability distributions consistent with NICER radii and 2-solar-mass limits.
-
Pulse profile modelling of the 2024 outburst of the accreting millisecond pulsar SRGA J144459.2-604207
Joint NICER+IXPE pulse-profile modeling of SRGA J144459.2-604207 favors large neutron-star mass and radius with two independent hotspots but shows strong sensitivity to joint-analysis methodology.
-
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.
-
Bayesian inferences on covariant density functionals from multimessenger astrophysical data: Influences of parametrizations of density dependent couplings
Different parametrizations of density dependence in covariant density functionals produce significant variations in the high-density equation of state and symmetry energy, with rational-function forms providing flexibility when saturation properties are adjusted and constrained by multimessenger ast
-
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}_{-0.0432} for a 1.4 M_⊙ star.
-
$f$-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.
-
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.
-
Hybrid stars among mass gap objects are excluded by twin stars at $1.4\,M_\odot$
Bayesian analysis of generic hybrid EOS with first-order deconfinement shows mass-gap hybrids require early transition and stiff quark matter, but data favor twins at 1.4 M_sun that exclude them.
-
The compact neutron star in 4U 1746-37 revisited: Reassessing the mass and radius
Significant X-ray flux blocking in 4U 1746-37 allows the neutron star to have canonical mass and radius values of 1.59 solar masses and 13 km or 2.12 solar masses and 9.8 km.
-
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.
-
Phase transitions in neutron stars and their links to gravitational waves
Review of neutron star dense matter, hadron-quark phase transitions, and potential g-mode signatures in gravitational waves from multimessenger observations.
-
Spin effects in superfluidity, neutron matter and neutron stars
A review of spin effects, superfluidity, and magnetic fields in neutron matter and their influence on neutron-star structure, superfluid phases, and rotational dynamics.