The effect of rotation on the stability of nuclear burning in accreting neutron stars

TL;DR

This study investigates how rotation and magnetic fields influence helium burning stability on neutron stars, revealing that magnetic instabilities enhance mixing, lowering the critical accretion rate for stable burning and explaining observed phenomena like oscillations.

Contribution

First detailed hydrodynamic models including rotation and magnetic fields show magnetic instabilities dominate mixing, affecting burning stability and matching observations.

Findings

Magnetic instabilities significantly enhance chemical mixing.

Rotation and magnetic fields lower the critical accretion rate for stable burning.

Oscillatory burning near the stability boundary explains observed QPO frequency drifts.

Abstract

Hydrogen and/or helium accreted by a neutron star from a binary companion may undergo thermonuclear fusion. At different mass accretion rates different burning regimes are discerned. Theoretical models predict helium fusion to proceed as a thermonuclear runaway for accretion rates below the Eddington limit and as stable burning above this limit. Observations, however, place the boundary close to 10% of the Eddington limit. We study the effect of rotationally induced transport processes on the stability of helium burning. For the first time detailed calculations of thin helium shell burning on neutron stars are performed using a hydrodynamic stellar evolution code including rotation and rotationally induced magnetic fields. We find that in most cases the instabilities from the magnetic field provide the dominant contribution to the chemical mixing, while Eddington-Sweet circulations become important at high rotation rates. As helium is diffused to greater depths, the stability of the burning is increased, such that the critical accretion rate for stable helium burning is found to be lower. Combined with a higher heat flux from the crust, as suggested by recent studies, turbulent mixing could explain the observed critical accretion rate. Furthermore, close to this boundary we find oscillatory burning, which previous studies have linked to mHz QPOs. In models where we continuously lower the heat flux from the crust, the period of the oscillations increases by up to several tens of percents, similar to the observed frequency drift, suggesting that this drift could be caused by the cooling of deeper layers.