Systematic numerical survey classifies four types of slow stable hybrid star branches and shows slow conversion opens new viable parameter space for stiff hadronic models.
Strong model-agnostic constraints for twin-star solutions
5 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
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2026 5representative citing papers
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.
Bayesian analysis favors a strong first-order phase transition in cold dense QCD matter whose onset lies above the central density of the most massive observed neutron stars.
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.
citing papers explorer
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Systematic study of the morphology and length of slow stable hybrid star branches
Systematic numerical survey classifies four types of slow stable hybrid star branches and shows slow conversion opens new viable parameter space for stiff hadronic models.
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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.
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On the Possibility of a Strong First-Order Phase Transition in Neutron Stars
Bayesian analysis favors a strong first-order phase transition in cold dense QCD matter whose onset lies above the central density of the most massive observed neutron stars.
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General gravitational properties of neutron stars: curvature invariants, binding energy, and trace anomaly
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.
- Hybrid stars among mass gap objects are excluded by twin stars at $1.4\,M_\odot$