Dependence of stellar magnetic activity cycles on rotational period in nonlinear solar-type dynamo

TL;DR

This study models how the rotation period of solar-type stars influences their magnetic activity cycles, incorporating nonlinear effects like magnetic helicity quenching and buoyancy to explain observed correlations.

Contribution

It introduces a nonlinear dynamo model that accounts for magnetic helicity quenching and buoyancy, explaining the dependence of activity cycle periods on stellar rotation.

Findings

Correlation between rotation period and activity cycle duration explained.

Nonlinear effects are crucial for accurate dynamo modeling.

Implications for understanding stellar magnetic activity processes.

Abstract

We study turbulent generation of large-scale magnetic fields using nonlinear dynamo models for solar-type stars in the range of rotational periods from 14 to 30 days. Our models take into account non-linear effects of dynamical quenching of magnetic helicity, and escape of magnetic field from the dynamo region due to magnetic buoyancy. The results show that the observed correlation between the period of rotation and the duration of activity cycles can be explained in the framework of a distributed dynamo model with a dynamical magnetic feedback acting on the turbulent generation either from magnetic buoyancy or magnetic helicity. We discuss implications of our findings for the understanding of dynamo processes operating in solar-like stars.