Core-crust transition pressure evolution in post-glitch epoch for a Vela-type pulsar

We propose that the \textit{post-glitch} epoch in a Vela-type pulsar corresponds to a transition time in which the broken \textit{crust} is readjusting its temperature and core-\textit{crust} transition pressure after the changes produced by the \textit{glitch}. To describe the evolution of the pulsar in this epoch we use a sequence of stationary and axisymmetric relativistic models of slowly rotating neutron stars with a surface layer \textit{crust}. Previously, we have formulated the matching conditions on the surface of the star in terms of physical properties (total mass of the star, core-\textit{crust} transition pressure,...).