  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 $P_t = (0.294 \pm 0.102)
MeV fm^{-3}$.
