Slow hadron-quark conversion in hybrid neutron stars creates extended stable 'waterfall' branches, reviving stiff hadronic equations of state that rapid-conversion analyses reject.
Komoltsev, Phys
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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.
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.
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.
citing papers explorer
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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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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.
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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.
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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.