Symmetry energy effects on location of the inner edge of neutron star crusts

TL;DR

This paper investigates how the symmetry energy influences the inner edge of neutron star crusts, highlighting potential errors in transition density and pressure calculations due to common approximations.

Contribution

It assesses the accuracy of the parabolic approximation in modeling the equation of state for asymmetric nuclear matter using three phenomenological models.

Findings

The parabolic approximation can lead to significant errors in transition density and pressure.

Errors in the approximation affect calculations of neutron star crust properties.

Results emphasize the need for more accurate models in neutron star studies.

Abstract

The symmetry energy effects on the location of the inner edge of neutron star crusts are studied. Three phenomenological models are employed in order to check the accuracy of the well known parabolic approximation of the equation of state for asymmetric nuclear matter in the determination of the transition density $n_t$ and transition pressure $P_t$. The results corroborate the statement that the error due to the assumption that a priori the equation of state is parabolic may introduce a large error in the determination of related properties of a neutron star as the crustal fraction of the moment of inertia and the critical frequency of rotating neutron stars.