Core-crust transition pressure for relativistic slowly rotating neutron stars

TL;DR

This paper investigates how variations in the core-crust transition pressure affect the structural and rotational properties of slowly rotating neutron stars using perturbation theory and matching conditions.

Contribution

It introduces a method to model neutron stars with variable core-crust transition pressure considering phase transitions and slow rotation effects.

Findings

Transition pressure influences neutron star mass and shape.

Phase transitions cause energy density jumps at the core-crust boundary.

Second-order perturbation theory captures deformation effects.

Abstract

We study the influence of core-\textit{crust} transition pressure changes on the general dynamical properties of neutron star configurations. First we study the matching conditions in core-\textit{crust} transition pressure region, where phase transitions in the equation of state causes energy density jumps. Then using a surface \textit{crust} approximation, we can construct configurations where the matter is described by the equation of state of the core of the star and the core-\textit{crust} transition pressure. We will consider neutron stars in the slow rotation limit, considering perturbation theory up to second order in the angular velocity so that the deformation of the star is also taken into account. The junction determines the parameters of the star such as total mass, angular and quadrupolar momentum.