PSR J0740+6620 has an equatorial radius of 13.7^{+2.6}_{-1.5} km, and multi-messenger data constrain 1.4 and 2.08 solar-mass neutron star radii to 12.45 and 12.35 km respectively.
Implications of PREX-II on the equation of state of neutron-rich matter
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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.
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.
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.
citing papers explorer
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The Radius of PSR J0740+6620 from NICER and XMM-Newton Data
PSR J0740+6620 has an equatorial radius of 13.7^{+2.6}_{-1.5} km, and multi-messenger data constrain 1.4 and 2.08 solar-mass neutron star radii to 12.45 and 12.35 km respectively.
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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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Characterizing the quark-hadron mixed phase in compact star cores : sensitivity to nuclear saturation and quark-model parameters at finite-temperature
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.
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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.