# Rossby and Magnetic Prandtl Number Scaling of Stellar Dynamos

## TL;DR

This paper investigates how stellar magnetic and kinetic energies scale with rotation and magnetic Prandtl number, comparing theoretical models with 3D dynamo simulations to understand energy balance and force-based dynamics.

## Contribution

It introduces and compares two scaling paradigms for stellar dynamos, validated against diverse 3D simulation data, enhancing understanding of magnetic energy behavior in stellar convection.

## Key findings

- Force-based scaling indicates a transition to magnetostrophic balance at low diffusion.
- Energy-balance scaling suggests a weaker dependence on convective Rossby number.
- Simulation data supports the applicability of both scaling regimes under different conditions.

## Abstract

Rotational scaling relationships are examined for the degree of equipartition between magnetic and kinetic energies in stellar convection zones. These scaling relationships are approached from two paradigms, with first a glance at scaling relationship built upon an energy-balance argument and second a look at a force-based scaling. The latter implies a transition between a nearly-constant inertial scaling when in the asymptotic limit of minimal diffusion and magnetostrophy, whereas the former implies a weaker scaling with convective Rossby number. Both scaling relationships are then compared to a suite of 3D convective dynamo simulations with a wide variety of domain geometries, stratifications, and range of convective Rossby numbers.