Bayesian analysis of NICER and small-radius pulsar data favors a strong first-order phase transition at 2.7-2.8 nuclear densities with a 600-700 MeV energy jump and high post-transition sound speed, producing twin stars of 6-7 km radius and strongly suppressed tidal deformability.
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Authors define U-spin symmetry energy for hyperonic matter, constrain it via Bayesian inference from nuclear and astrophysical data, and conclude Lambda hyperons likely emerge between 2-5 n0 but vanish above 5 n0 with over 50% posterior probability.
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Bayesian Inference of Dense-Matter Equations of State from Small-Radius Compact Stars with Twin-Star Scenarios
Bayesian analysis of NICER and small-radius pulsar data favors a strong first-order phase transition at 2.7-2.8 nuclear densities with a 600-700 MeV energy jump and high post-transition sound speed, producing twin stars of 6-7 km radius and strongly suppressed tidal deformability.
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U-spin symmetry energy and hyperon puzzle
Authors define U-spin symmetry energy for hyperonic matter, constrain it via Bayesian inference from nuclear and astrophysical data, and conclude Lambda hyperons likely emerge between 2-5 n0 but vanish above 5 n0 with over 50% posterior probability.