Magnetic coronae of active main-sequence stars

TL;DR

This paper reviews recent advances in understanding the complex and diverse coronal structures of active main-sequence stars, highlighting differences from the solar corona influenced by stellar rotation and internal structure.

Contribution

It provides new insights into how stellar internal structure and rotation affect coronal geometry, dynamics, and emissions in active main-sequence stars.

Findings

Active stars show non-solar coronal behaviors.

Coronal structure varies with stellar rotation and internal structure.

Recent observations reveal diverse coronal geometries.

Abstract

The coronal structure of main sequence stars continues to puzzle us. While the solar corona is relatively well understood, it has become clear that even stars of the same mass as the Sun can display very non-solar coronal behaviour, particularly if they are rapid rotators or in a binary system. At masses greater than and also less than that of the Sun, the non-solar internal structure appears to affect both the geometry and dynamics of the stellar corona and the nature of the X-ray and radio emission. In this talk I will describe some recent advances in our understanding of the structure of the coronae of some of the most active (and interesting) main sequence stars.