Thermal convection in rotating spherical shells: temperature-dependent internal heat generation using the example of triple-$\alpha$ burning in neutron stars

TL;DR

This study uses 3D simulations to analyze how temperature-dependent internal heating influences thermal convection in rotating spherical shells, with implications for neutron star ocean dynamics and thermonuclear burst evolution.

Contribution

It introduces a dimensionless parameter for nuclear heating relevance and explores flow regime transitions in convection with temperature-dependent internal heat sources.

Findings

Flow characteristics change with increasing nuclear heating parameter.

Onset of convection depends on nuclear heating strength.

Various flow regimes, including turbulent states, are identified.

Abstract

We present an extensive study of Boussinesq thermal convection including a temperature-dependent internal heating source, based on numerical three-dimensional simulations. The temperature dependence mimics triple-$\alpha$ nuclear reactions and the fluid geometry is a rotating spherical shell. These are key ingredients for the study of convective accreting neutron star oceans. A dimensionless parameter ${{\rm Ra}}_n$, measuring the relevance of nuclear heating, is defined. We explore how flow characteristics change with increasing ${{\rm Ra}}_n$ and give an astrophysical motivation. The onset of convection is investigated with respect to this parameter and periodic, quasiperiodic, chaotic flows with coherent structures, and fully turbulent flows are exhibited as ${{\rm Ra}}_n$ is varied. Several regime transitions are identified and compared with previous results on differentially heated convection. Finally, we explore (tentatively) the potential applicability of our results to the evolution of thermonuclear bursts in accreting neutron star oceans.