Turbulent effects are argued to be essential for dynamos in the Sun and stars. While inaccessible observationally, they can be directly studied using global convective dynamo (GCD) simulations. We measure these turbulent effects, in terms of turbulent transport coefficients, from an exemplary GCD simulation using the test-field method. These coefficients are then used as an input into a mean-field (MF) model. We find a good agreement between the MF and GCD solutions, which validates our theoretical approach. This agreement requires all turbulent effects to be included, even those which have been regarded unimportant so far. Our results suggest that simple dynamo models as are commonly used in the solar and stellar community, relying on very few, precisely fine-tuned turbulent effects, may not be representative of the full dynamics of GCDs in astronomical objects.
|Journal||Astrophysical Journal Letters|
|Publication status||Submitted - 1 May 2021|
|MoE publication type||A1 Journal article-refereed|
- Astrophysics - Solar and Stellar Astrophysics
- Physics - Fluid Dynamics