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 isovector compressibility K _ { sym } and skewness Q _ { sym } have the most significant correlations with the transition point , along with the previously observed influence of the L _ { sym } parameter .
The estimated density and pressure of the crust-core transition are n _ { t } = ( 0.071 \pm 0.011 ) fm ^ { -3 } and P _ { t } = ( 0.294 \pm 0.102 ) MeVfm ^ { -3 } .