Estimations and scaling laws for stellar magnetic fields

TL;DR

This paper derives and validates scaling laws for stellar magnetic fields influenced by rotation, using simplified dynamo equations and turbulence theory, aligning well with observational data.

Contribution

It introduces new scaling laws for stellar magnetic fields based on simplified dynamo models and turbulence theory, accounting for different rotation regimes.

Findings

Scaling laws agree with observational data

Magnetic field dependence on rotation rate

Simplified dynamo equations effectively model stellar magnetism

Abstract

In rapidly rotating turbulence (Rossby number much less than unity), the standard mixing length theory for turbulent convection breaks and Coriolis force enters the force balance such that magnetic field eventually depends on rotation. By simplifying the self-sustained magnetohydrodynamics dynamo equations of electrically conducting fluid motion, with the aid of theory of isotropic non-rotating or anisotropic rotating turbulence driven by thermal convection, we make estimations and derive scaling laws for stellar magnetic fields with slow and fast rotation. Our scaling laws are in good agreement with the observations.