Numerical simulation of convection in K dwarfs

TL;DR

This study uses numerical simulations to analyze convection, differential rotation, meridional flows, and magnetic field generation in a 0.7 solar mass K dwarf star rotating at the solar period.

Contribution

It provides new insights into the convection patterns and magnetic field behavior in K dwarfs with solar-like rotation, highlighting differences from the Sun.

Findings

Differential rotation is solar-type despite rapid rotation.

A large-scale magnetic field is generated but lacks a simple cycle.

The star's convection and magnetic properties differ from solar observations.

Abstract

We have carried out numerical simulations of the convection zone in a K dwarf of 0.7 solar masses rotating at the solar rotation period. We study the convection pattern, the differential rotation and meridional flows, and the dynamo-generated magnetic field. We find that for a star of this type, the solar rotation period represents a case of fairly rapid rotation and the differential is solar-type. A dynamo-generated large scale field appears but it is neither dipolar nor does it show a simple activity cycle.