Stellar mass ejections

It has been known for some time now that, rapidly-rotating solar-like stars possess the stellar equivalent of solar prominences. These may be three orders of magnitude more massive than their solar counterparts, and their ejection from the star may form a significant, contribution to the loss of angular momentum and nuts's ill the Stellar wind. In addition, their number and distribution provide valuable cities as to the structure of the stellar corolla and hence to the nature of magnetic activity in other stars.

Until recently, these "slingshot prominences" had only been observed in mature stars, but their recent detection in an extremely young star suggests that they may be, more widespread than previously thought. In this review we will summarise our current understanding of these stellar prominences, their ejection front their stars and their role in elucidating the (sometimes very non-solar) behaviour of stellar magnetic fields.