New model of relativistic slowly rotating neutron stars with surface layer \textit{crust}: application to giant \textit{glitches} of Vela Pulsar

TL;DR

This paper develops a new relativistic model of slowly rotating neutron stars with a surface crust layer, explaining giant glitches in the Vela pulsar through variations in transition pressure.

Contribution

It introduces a formalism incorporating a surface crust layer and analyzes how transition pressure variations can cause pulsar glitches.

Findings

Transition pressure variations can explain Vela pulsar glitches.

Model aligns crust temperature changes with glitch phenomena.

Provides a new framework for neutron star surface layer analysis.

Abstract

Introducing a surface layer of matter on the edge of a neutron star in slow rigid rotation, we analyze, from an intrinsic point of view, the junction conditions that must be satisfied between the interior and exterior solutions of the Einstein equations. In our model the core-\textit{crust} transition pressure arise as an essential parameter in the description of a configuration. As an application of this formalism, we describe giant \textit{glitches} of the Vela pulsar as a result of variations in the transition pressure, finding that these small changes are compatible with the expected temperature variations of the inner crust during \textit{glitch} time.