Deep Crustal Heating in a Multicomponent Accreted Neutron Star Crust

TL;DR

This paper models the multicomponent composition and deep crustal heating in accreting neutron stars using a quasi-statistical equilibrium approach, highlighting the impact of nuclear symmetry energy uncertainties.

Contribution

It introduces a comprehensive model that simulates the crust composition and heating processes, incorporating nuclear shell effects and reaction pathways.

Findings

Nuclear symmetry energy significantly affects crustal heating.

Reaction pathways are consistent with a liquid droplet nuclear mass model.

Deep crustal heating varies by up to a factor of two with symmetry energy changes.

Abstract

A quasi-statistical equilibrium model is constructed to simulate the multicomponent composition of the crust of an accreting neutron star. The ashes of rp-process nucleosynthesis are driven by accretion through a series of electron captures, neutron emissions, and pycnonuclear fusions up to densities near the transition between the neutron star crust and core. A liquid droplet model which includes nuclear shell effects is used to provide nuclear masses far from stability. Reaction pathways are determined consistently with the nuclear mass model. The nuclear symmetry energy is an important uncertainty in the masses of the exotic nuclei in the inner crust and varying the symmetry energy changes the amount of deep crustal heating by as much as a factor of two.