Magnetic Fields on Cool Stars

TL;DR

This paper reviews methods for measuring magnetic fields in cool stars, compares results for M-type stars, and discusses the diversity of magnetic geometries and the need for further observational and theoretical work.

Contribution

It provides a comparative overview of two main measurement techniques for stellar magnetic fields and highlights the current understanding and gaps in interpreting magnetic geometries in cool stars.

Findings

Magnetic fields in active M-type stars are typically a few kG.

Two main measurement methods are polarized light and Zeeman broadening.

Magnetic geometries show great diversity with no clear dynamo picture yet.

Abstract

Magnetic fields are an important ingredient to cool star physics, and there is great interest in measuring fields and their geometry in order to understand stellar dynamos and their influence on star formation and stellar evolution. During the last few years, a large number of magnetic field measurements became available. Two main approaches are being followed to measure the Zeeman effect in cool stars; 1) the measurement of polarized light, for example to produce magnetic maps, and 2) the measurement of integrated Zeeman broadening to measure the average magnetic field strength on the stellar surface. This article briefly reviews the two methods and compares results between them that are now available for about a dozen M-type stars. It seems that we see a great variety of magnetic geometries and field strengths with typical average fields of a few kG in active M-type stars. The interpretation of geometries, however, has not yet led to a clear picture of magnetic dynamos and field configuration, and work is needed on more observational data but also on the fundamental understanding of our measurements.