  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 mass in the stellar wind. In addition, their number and
distribution provide valuable clues as to the structure of the stellar corona
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 I will
summarise our current understanding of these stellar prominences, their
ejection from their stars and their role in elucidating the (sometimes very
non-solar) behaviour of stellar magnetic fields.
