  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.
