Core-crust transition pressure evolution in post-glitch epoch for a Vela-type pulsar
Abstract
We propose that the post-glitch epoch in a Vela-type pulsar corresponds to a transition time in which the broken crust is readjusting its temperature and core-crust transition pressure after the changes produced by the 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 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-crust transition pressure,...).
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