Magnetized oscillatory double-diffusive convection

TL;DR

This study investigates how a vertical magnetic field influences oscillatory double-diffusive convection in stellar regions, revealing that magnetic fields modify turbulence, delay layer formation, and may suppress convection entirely at high strengths.

Contribution

It provides the first analysis of magnetic effects on ODDC, showing quantitative differences in instability saturation and layer formation compared to non-magnetic cases.

Findings

Magnetic fields reduce turbulent fluxes of temperature and composition.

Magnetic fields can delay or suppress layer formation.

Fastest-growing modes are unaffected by magnetic fields.

Abstract

We study the properties of oscillatory double-diffusive convection (ODDC) in the presence of a uniform vertical background magnetic field. ODDC takes place in stellar regions that are unstable according to the Schwarzschild criterion and stable according to the Ledoux criterion (sometimes called semiconvective regions), which are often predicted to reside just outside the core of intermediate-mass main sequence stars. Previous hydrodynamic studies of ODDC have shown that the basic instability saturates into a state of weak wave-like convection, but that a secondary instability can sometimes transform it into a state of layered convection, where layers then rapidly merge and grow until the entire region is fully convective. We find that magnetized ODDC has very similar properties overall, with some important quantitative differences. A linear stability analysis reveals that the fastest-growing modes are unaffected by the field, but that other modes are. Numerically, the magnetic field is seen to influence the saturation of the basic instability, overall reducing the turbulent fluxes of temperature and composition. This in turn affects layer formation, usually delaying it, and occasionally suppressing it entirely for sufficiently strong fields. Further work will be needed, however, to determine the field strength above which layer formation is actually suppressed in stars. Potential observational implications are briefly discussed.