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.
Quarkyonic Matter and Neutron Stars
11 Pith papers cite this work. Polarity classification is still indexing.
11
Pith papers citing it
abstract
We consider Quarkyonic Matter to naturally explain the observed properties of neutron stars. We argue that such matter might exist at densities close to that of nuclear matter and at the onset, the pressure and the sound velocity in Quarkyonic matter increase rapidly. In the limit of large number of quark colors $N_c$, this transition is characterized by a discontinuous change in pressure as a function of baryon number density. We make a simple model of Quarkyonic matter and show that generically the sound velocity is a non-monotonic function of density -- it reaches a maximum at relatively low density, decreases, and then increases again to its asymptotic value of $1/\sqrt{3}$.
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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.
Slow hadron-quark conversion in hybrid neutron stars creates extended stable 'waterfall' branches, reviving stiff hadronic equations of state that rapid-conversion analyses reject.
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.
A quark-meson model with lattice-fitted temperature-dependent quark masses and anomalous magnetic moments reproduces the magnetic susceptibility of hot hadronic matter up to the QCD crossover, showing quarks are active below 120 MeV.
In large-Nc QCD at finite isospin density, an intermediate regime Lambda_QCD <= mu_I <= sqrt(Nc) Lambda_QCD hosts quarkyonic meson matter consisting of a filled Fermi sea of quarks bound into mesons on the QCD scale, possibly with surface Bose condensation or Cooper pairing.
The IdylliQ model uses quark saturation to generate stiff equations of state and effective baryon repulsions that mitigate hyperon softening in neutron star matter.
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.
In the modified NJL model, low vacuum pressure with a first-order chiral transition supports massive non-strange quark stars consistent with pulsar data while high vacuum pressure with crossover is ruled out, constraining current quark mass to 4.08-4.13 MeV and suggesting GW170817 could involve such
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.
A unified QCD equation of state is advocated for neutron star mergers and heavy ion collisions so that gravitational wave signals and lab flow/fluctuation data can jointly constrain the phase structure of dense matter.
citing papers explorer
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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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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.
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Systematic study of the morphology and length of slow stable hybrid star branches
Slow hadron-quark conversion in hybrid neutron stars creates extended stable 'waterfall' branches, reviving stiff hadronic equations of state that rapid-conversion analyses reject.
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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.
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Magnetic susceptibility of a hot hadronic medium and quark degrees of freedom near the QCD cross-over point
A quark-meson model with lattice-fitted temperature-dependent quark masses and anomalous magnetic moments reproduces the magnetic susceptibility of hot hadronic matter up to the QCD crossover, showing quarks are active below 120 MeV.
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Quarkyonic Meson Matter for Finite Isospin Density
In large-Nc QCD at finite isospin density, an intermediate regime Lambda_QCD <= mu_I <= sqrt(Nc) Lambda_QCD hosts quarkyonic meson matter consisting of a filled Fermi sea of quarks bound into mesons on the QCD scale, possibly with surface Bose condensation or Cooper pairing.
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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.
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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.
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QCD vacuum pressure and its influence on the equation of state of non-strange quark stars
In the modified NJL model, low vacuum pressure with a first-order chiral transition supports massive non-strange quark stars consistent with pulsar data while high vacuum pressure with crossover is ruled out, constraining current quark mass to 4.08-4.13 MeV and suggesting GW170817 could involve such
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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.
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Matter And Gravitation In Collisions of heavy ions and neutron stars: equation of state
A unified QCD equation of state is advocated for neutron star mergers and heavy ion collisions so that gravitational wave signals and lab flow/fluctuation data can jointly constrain the phase structure of dense matter.