Magnetized oscillatory double-diffusive convection

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.

arXiv comment24 pages, single column, 6 figures, accepted for publication in ApJ

References in corpus (17)

• Modules for Experiments in Stellar Astrophysics (MESA)
• Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions
• Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation
• Numerically determined transport laws for fingering ("thermohaline") convection in astrophysics
• A new model for mixing by double-diffusive convection (semi-convection): I. The conditions for layer formation
• Turbulent mixing and layer formation in double-diffusive convection: 3D numerical simulations and theory
• A new model for mixing by double-diffusive convection (semi-convection). II. The transport of heat and composition through layers
• The Magnetic Furnace: Intense Core Dynamos in B-stars
• Dynamics of fingering convection I: Small-scale fluxes and large-scale instabilities
• On the proper use of the Schwarzschild and Ledoux criteria in stellar evolution computations
• Dynamics of fingering convection II: The formation of thermohaline staircases
• Excitation of gravity waves by fingering convection, and the formation of compositional staircases in stellar interiors
• Enhanced mixing in magnetized fingering convection, and implications for RGB stars
• A New Model for Mixing By Double-Diffusive Convection (Semi-Convection). III. Thermal and Compositional Transport Through Non-Layered ODDC
• Main Sequence Evolution with Layered Semiconvection
• Fingering convection induced by atomic diffusion in stars: 3D numerical computations and applications to stellar models
• Schwarzschild and Ledoux are equivalent on evolutionary timescales