Abstract
The influence of the uncertainties of the equation of state empirical parameters on the neutron stars crust-core phase transition is explored within a meta-modeling approach, in which the energy per particle is expanded as a Taylor series in density and asymmetry around the saturation point. The phase transition point is estimated from the intersection of the spinodal instability region for dynamical fluctuations with the chemical equilibrium curve. Special attention is paid to the inclusion of high-order parameters of the Taylor series and their influence on the transition point. An uncorrelated prior distribution is considered for the empirical parameters, with bulk properties constrained through effective field theory predictions, while the surface parameters are controlled from a fit of nuclear masses using the extended Thomas Fermi approximation. The results show that the isospin dependent curvature Ksym and skewness Qsym have the most significant correlations with the transition point, along with the well known influence of the Lsym parameter. The estimated density and pressure of the crust-core transition are nt = (0.071 ± 0.011) fm−3 and Pt = (0.294 ±0.102) MeV fm−3.
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