Using a parity doublet hadronic model, an NJL quark model, and integral causality constraints, the paper finds that the maximum allowed first-order phase-transition density jump in neutron-star matter decreases as the chiral invariant mass m0 increases.
Microscopic nuclear equation of state with three-body forces and neutron star structure
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abstract
We calculate static properties of non-rotating neutron stars (NS's) using a microscopic equation of state (EOS) for asymmetric nuclear matter, derived from the Brueckner-Bethe-Goldstone many-body theory with explicit three-body forces. We use the Argonne AV14 and the Paris two-body nuclear force, implemented by the Urbana model for the three-body force. We obtain a maximum mass configuration with $ M_{max} = 1.8 M_{\sun}$ ($M_{max} = 1.94 M_{\sun}$) when the AV14 (Paris) interaction is used. They are both consistent with the observed range of NS masses. The onset of direct Urca processes occurs at densities $n \geq 0.65~fm^{-3}$ for the AV14 potential and $n \geq 0.54~fm^{-3}$ for the Paris potential. Therefore, NS's with masses above $M^{Urca} = 1.4 M_{\sun}$ for the AV14 and $M^{Urca} = 1.24 M_{\sun}$ for the Paris potential can undergo very rapid cooling, depending on the strength of superfluidity in the interior of the NS. The comparison with other microscopic models for the EOS shows noticeable differences.
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Constraints on the strength of first-order phase transition and its relation to nucleon mass
Using a parity doublet hadronic model, an NJL quark model, and integral causality constraints, the paper finds that the maximum allowed first-order phase-transition density jump in neutron-star matter decreases as the chiral invariant mass m0 increases.