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

TL;DR

This paper models the post-glitch epoch in Vela-type pulsars as a transition period where the crust readjusts its temperature and transition pressure, using relativistic models of rotating neutron stars with a crust.

Contribution

It introduces a new approach to describe the post-glitch evolution by applying relativistic models with a surface crust layer and matching conditions based on physical properties.

Findings

Model describes crust temperature and transition pressure evolution after glitches.

Relativistic models incorporate crust and core properties for pulsar evolution.

Provides a framework for understanding post-glitch neutron star dynamics.

Abstract

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,...).