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.
Trace Anomaly as Signature of Con- formality in Neutron Stars,
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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.
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.
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.
DM admixture in isentropic neutron stars can mimic quark-matter conformality signatures via competition between thermal effects and dark sector softening.
Slow strong hadron-quark phase transitions allow stable hybrid-star branches that accommodate both high-mass and low-radius observations in two viable patterns from a parameter scan.
The quark-hadron mixed phase width in hybrid stars is mainly controlled by effective nucleon mass and symmetry energy, with temperature reducing the width and softening the EOS while strong vector repulsion is needed to match massive pulsar and NICER data.
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.
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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Can a Slow and Strong Phase Transition in Neutron Stars Relieve Major Compact-Star Observation Tensions?
Slow strong hadron-quark phase transitions allow stable hybrid-star branches that accommodate both high-mass and low-radius observations in two viable patterns from a parameter scan.