Simulations of solar and stellar dynamos and their theoretical interpretation

TL;DR

This paper reviews advanced 3D numerical simulations of solar and stellar dynamos, discussing their constraints, observational comparisons, and theoretical interpretations, highlighting the role of rotation and mean-field theory in magnetic activity.

Contribution

It provides a comprehensive overview of current simulation techniques, their limitations, and how they relate to observations and mean-field dynamo theory, advancing understanding of stellar magnetic phenomena.

Findings

Rotation influences magnetic activity levels.

Simulations replicate observed large-scale magnetic fields.

Mean-field theory helps interpret complex simulation results.

Abstract

We review the state of the art of three dimensional numerical simulations of solar and stellar dynamos. We summarize fundamental constraints of numerical modelling and the techniques to alleviate these restrictions. Brief summary of the relevant observations that the simulations seek to capture is given. We survey the current progress of simulations of solar convection and the resulting large-scale dynamo. We continue to studies that model the Sun at different ages and to studies of stars of different masses and evolutionary stages. Both simulations and observations indicate that rotation, measured by the Rossby number which is the ratio of rotation period and convective turnover time, is a key ingredient in setting the overall level and characteristics of magnetic activity. Finally, efforts to understand global 3D simulations in terms of mean-field dynamo theory are discussed.