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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Diquark coupling in the NJL model is fixed near 1.5 times the scalar coupling and vector coupling below 1.1 times, yielding crossover equations of state that raise maximum neutron star masses and produce distinct radial oscillation frequencies potentially detectable as quark-matter signatures.
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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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Crossover Equation of State Constrained by Astronomical Observations and pQCD
Diquark coupling in the NJL model is fixed near 1.5 times the scalar coupling and vector coupling below 1.1 times, yielding crossover equations of state that raise maximum neutron star masses and produce distinct radial oscillation frequencies potentially detectable as quark-matter signatures.