Mean-Field Modeling of $\alpha^2$-Dynamo Coupled with Direct Numerical Simulations of Rigidly Rotating Convection

TL;DR

This study combines direct numerical simulations and mean-field modeling to demonstrate that oscillatory $$ dynamo waves driven by nonuniform $$-effects in rotating stratified convection can explain large-scale stellar magnetic phenomena.

Contribution

The paper introduces a mean-field dynamo model based on DNS data, showing that $$ dynamos can operate without the $$-effect in rotating convection.

Findings

Oscillatory $$ dynamo waves are responsible for magnetic cycles.

Nonuniform $$-effects are crucial for large-scale dynamo action.

Model results match DNS observations of magnetic field migration.

Abstract

The mechanism of large-scale dynamos in rigidly rotating stratified convection is explored by direct numerical simulations (DNS) in Cartesian geometry. A mean-field dynamo model is also constructed using turbulent velocity profiles consistently extracted from the corresponding DNS results. By quantitative comparison between the DNS and our mean-field model, it is demonstrated that the oscillatory $\alpha^2$ dynamo wave, excited and sustained in the convection zone, is responsible for large-scale magnetic activities such as cyclic polarity reversal and spatiotemporal migration. The results provide strong evidence that a nonuniformity of the $\alpha$-effect, which is a natural outcome of rotating stratified convection, can be an important prerequisite for large-scale stellar dynamos, even without the $\Omega$-effect.