Develops a local open EFT for non-Abelian gauge theories using dynamical color-frame variables and color-current sectors in Schwinger-Keldysh formalism, yielding nonlocal dissipative kernels and naturally incorporating hard thermal loop responses after integration.
hub Canonical reference
From hadrons to quarks in neutron stars: a review
Canonical reference. 100% of citing Pith papers cite this work as background.
29
Pith papers citing it
Background
100% of classified citations
abstract
We review the equation of state of matter in neutron stars from the solid crust through the liquid nuclear matter interior to the quark regime at higher densities. We focus in detail on the question of how quark matter appears in neutron stars, and how it affects the equation of state. After discussing the crust and liquid nuclear matter in the core we briefly review aspects of microscopic quark physics relevant to neutron stars, and quark models of dense matter based on the Nambu--Jona-Lasinio framework, in which gluonic processes are replaced by effective quark interactions. We turn then to describing equations of state useful for interpretation of both electromagnetic and gravitational observations, reviewing the emerging picture of hadron-quark continuity in which hadronic matter turns relatively smoothly, with at most only a weak first order transition, into quark matter with increasing density. We review construction of unified equations of state that interpolate between the reasonably well understood nuclear matter regime at low densities and the quark matter regime at higher densities. The utility of such interpolations is driven by the present inability to calculate the dense matter equation of state in QCD from first principles. As we review, the parameters of effective quark models -- which have direct relevance to the more general structure of the QCD phase diagram of dense and hot matter -- are constrained by neutron star mass and radii measurements, in particular favoring large repulsive density-density and attractive diquark pairing interactions. We describe the structure of neutron stars constructed from the unified equations of states with crossover. Lastly we present the current equations of state -- called "QHC18" for quark-hadron crossover -- in a parametrized form practical for neutron star modeling.
hub tools
citation-role summary
background 11
citation-polarity summary
roles
background 11polarities
background 11representative citing papers
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.
Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable stars.
A first-principles FRG approach to two-flavor QCD derives low-energy constants for the pion, sigma-meson and scalar diquark without parameters beyond QCD itself, including new diquark properties for color-superconducting models.
Accretion-induced failure of the neutron star crystal crust produces a glass layer that explains the observed cooling, fixes the accreted mass at 2.4e-6 solar masses, and indicates birth properties typical of recycled neutron stars, potentially from electron-capture supernova formation.
Bayesian analysis of astrophysical and laboratory data favors the two-families scenario of coexisting hadronic and strange quark stars over the one-family scenario.
X-ray timing and spectral analysis of ASKAP J174508.9-505149 detects matching periodicity and features consistent with an accreting magnetic CV.
Causal viscous relativistic hydrodynamics applied to neutron stars yields new axial mode families without perfect-fluid counterparts, including mode avoidance and long-lived modes.
Large initial baryon asymmetry allows Hubble patches to collapse into primordial neutron stars arrested by nuclear pressure, requiring later entropy dilution to match observed Y_B and BBN.
RMF-CC models with ωρ coupling better match multi-messenger NS data and LQCD/NEP constraints than the baseline, yet standard RMF remains preferred without core phase transitions, requiring high Ksat ~300 MeV.
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.
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-percent level.
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.
Dissipative protocols on quantum hardware prepare approximate thermal states for kagome AFIM up to 79 sites and AFHM via simulation, with circuit depth independent of size and linear in inverse temperature.
Mass-gap compact objects could be hybrid stars only with very early deconfinement and stiff quark matter; confirming 1.4 M⊙ twin stars would cap hybrid-star maximum mass below 2.2 M⊙.
NLED alters photon propagation near magnetars, producing ~10% errors in inferred radii via ray-tracing and a minimal ~350 ns travel-time delay.
Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.
Hybrid star model with core quark pasta pinning superfluid vortices produces glitch amplitudes ΔΩ/Ω of order 10^{-6} matching Vela-like pulsar observations.
Steep matter-density gradients in neutron stars can produce neutrino-antineutrino pairs analogous to the Schwinger effect.
Hybrid neutron-star equations of state remain sensitive to the low-density nucleonic model at transition densities around 2ρ₀, with model spread in radius and tidal deformability exceeding observational uncertainty by factors of ~1.8 and ~1.4.
FRG analysis in the linear sigma model for QC2D shows enhanced meson U(1)_A anomaly couplings with increasing mu_q but suppressed topological susceptibility following chiral restoration at high density or temperature.
The IdylliQ model uses quark saturation to generate stiff equations of state and effective baryon repulsions that mitigate hyperon softening in neutron star matter.
An extended linear sigma model with delta meson and negative sigma_piN produces a symmetry-energy plateau and stiffer EOS that satisfies neutron-star and nuclear constraints.
Neutrino light curves from neutron stars may show an enhanced peak-to-plateau ratio, a density-tracing delay, and transient spectral hardening as diagnostics of hadron-quark phase transitions on 10-50 ms timescales.
citing papers explorer
-
Bottom-up open EFT for non-Abelian gauge theory with dynamical color environment
Develops a local open EFT for non-Abelian gauge theories using dynamical color-frame variables and color-current sectors in Schwinger-Keldysh formalism, yielding nonlocal dissipative kernels and naturally incorporating hard thermal loop responses after integration.
-
Bayesian Constraints on the Neutron Star Equation of State with a Smooth Hadron-Quark Crossover
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.
-
As above, so below: assessing extremeness of the neutron-star equation of state based on the unstable branch
Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable stars.
-
Scalar diquarks in the QCD vacuum
A first-principles FRG approach to two-flavor QCD derives low-energy constants for the pion, sigma-meson and scalar diquark without parameters beyond QCD itself, including new diquark properties for color-superconducting models.
-
Crust glass formation reveals the neutron star birth properties in IGR J17480-2446
Accretion-induced failure of the neutron star crystal crust produces a glass layer that explains the observed cooling, fixes the accreted mass at 2.4e-6 solar masses, and indicates birth properties typical of recycled neutron stars, potentially from electron-capture supernova formation.
-
Is the coexistence of strange quark stars and hadronic stars favored by astrophysical data? A Bayesian analysis
Bayesian analysis of astrophysical and laboratory data favors the two-families scenario of coexisting hadronic and strange quark stars over the one-family scenario.
-
The X-ray emission of the long-period transient and accreting cataclysmic variable ASKAP J174508.9-505149
X-ray timing and spectral analysis of ASKAP J174508.9-505149 detects matching periodicity and features consistent with an accreting magnetic CV.
-
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.
-
Primordial Neutron Stars
Large initial baryon asymmetry allows Hubble patches to collapse into primordial neutron stars arrested by nuclear pressure, requiring later entropy dilution to match observed Y_B and BBN.
-
Relativistic Mean Field Approach with Chiral Symmetry Breaking and Quark Confinement in the light of Astrophysical Observations
RMF-CC models with ωρ coupling better match multi-messenger NS data and LQCD/NEP constraints than the baseline, yet standard RMF remains preferred without core phase transitions, requiring high Ksat ~300 MeV.
-
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.
-
The crust of dark-matter admixed neutron stars: bulk properties and torsional oscillations
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-percent level.
-
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.
-
Preparing thermal states of frustrated quantum spin systems using 139 qubits
Dissipative protocols on quantum hardware prepare approximate thermal states for kagome AFIM up to 79 sites and AFHM via simulation, with circuit depth independent of size and linear in inverse temperature.
-
Hybrid stars among mass gap objects are excluded by twin stars at $1.4\,M_\odot$
Mass-gap compact objects could be hybrid stars only with very early deconfinement and stiff quark matter; confirming 1.4 M⊙ twin stars would cap hybrid-star maximum mass below 2.2 M⊙.
-
Nonlinear electrodynamics in magnetars: systematic effects on radius constraints and timing analysis
NLED alters photon propagation near magnetars, producing ~10% errors in inferred radii via ray-tracing and a minimal ~350 ns travel-time delay.
-
Nucleosynthesis in the fast ejecta of a neutron star merger
Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.
-
Modeling large glitches with core superfluidity in a Hybrid star
Hybrid star model with core quark pasta pinning superfluid vortices produces glitch amplitudes ΔΩ/Ω of order 10^{-6} matching Vela-like pulsar observations.
-
Gradient-Produced Neutrinos
Steep matter-density gradients in neutron stars can produce neutrino-antineutrino pairs analogous to the Schwinger effect.
-
Sensitivity of Neutron Star Observables to Transition Density in Hybrid Equation-of-State Models
Hybrid neutron-star equations of state remain sensitive to the low-density nucleonic model at transition densities around 2ρ₀, with model spread in radius and tidal deformability exceeding observational uncertainty by factors of ~1.8 and ~1.4.
-
FRG analysis of dense two-color QCD within the linear sigma model
FRG analysis in the linear sigma model for QC2D shows enhanced meson U(1)_A anomaly couplings with increasing mu_q but suppressed topological susceptibility following chiral restoration at high density or temperature.
-
A quarkyonic matter model
The IdylliQ model uses quark saturation to generate stiff equations of state and effective baryon repulsions that mitigate hyperon softening in neutron star matter.
-
Nuclear matter properties and neutron star structures from an extended linear sigma model
An extended linear sigma model with delta meson and negative sigma_piN produces a symmetry-energy plateau and stiffer EOS that satisfies neutron-star and nuclear constraints.
-
Neutrino diagnostics of hadron-quark phase transition in Neutron Stars
Neutrino light curves from neutron stars may show an enhanced peak-to-plateau ratio, a density-tracing delay, and transient spectral hardening as diagnostics of hadron-quark phase transitions on 10-50 ms timescales.
-
Hot quark matter and (proto-) neutron stars
An extended PNJL model locates the QCD critical end point and predicts that proto-neutron stars contain hyperons and Delta-isobars but no deconfined quarks, which appear only in cold neutron stars.
-
A Poincar\'e-covariant study of strange quark stars
A Poincaré-covariant vector-vector contact interaction yields an equation of state for strange quark matter whose mass-radius and tidal properties match pulsar and gravitational-wave constraints for two tuned parameter sets.
-
Two Lectures on the Phase Diagram of QCD
QCD features at least three phases at zero baryon density and three at high density, including a Quarkyonic phase at high density and low temperature, described via large-N_c and a parameter-free 3D string model.
-
Studying the QCD Matter produced in Heavy-Ion Collisions using the MUSES Calculation Engine
The MUSES Calliope engine computes multi-dimensional QCD equations of state, merges them consistently, and feeds them into viscous hydrodynamic simulations of heavy-ion collisions with movable critical points and critical scaling in transport coefficients.
-
Science Case for the Einstein Telescope
The Einstein Telescope will enable gravitational-wave observations up to cosmological distances, opening avenues for discoveries in astrophysics, cosmology, and fundamental physics.