(Simulating) Coronal Mass Ejections in Active Stars

TL;DR

This paper presents 3D simulations of coronal mass ejections in active stars, comparing them with solar eruptions, and explores potential observable signatures in M-dwarf stars to improve understanding of stellar eruptive phenomena.

Contribution

It introduces the first 3D CME simulations for M-dwarf stars and offers a unified framework to interpret stellar CME observations.

Findings

Simulated properties of stellar CMEs differ from solar eruptions.

Potential observable signatures in M-dwarf stellar coronae identified.

Provides a basis for future observational validation of stellar CMEs.

Abstract

The stellar magnetic field completely dominates the environment around late-type stars. It is responsible for driving the coronal high-energy radiation (e.g. EUV/X-rays), the development of stellar winds, and the generation transient events such as flares and coronal mass ejections (CMEs). While progress has been made for the first two processes, our understanding of the eruptive behavior in late-type stars is still very limited. One example of this is the fact that despite the frequent and highly energetic flaring observed in active stars, direct evidence for stellar CMEs is almost non-existent. Here we discuss realistic 3D simulations of stellar CMEs, analyzing their resulting properties in contrast with solar eruptions, and use them to provide a common framework to interpret the available stellar observations. Additionally, we present results from the first 3D CME simulations in M-dwarf stars, with emphasis on possible observable signatures imprinted in the stellar corona.