  Observations of rapidly-rotating cool stars often show coronal slingshot
prominences that remove mass and angular momentum when they are ejected. The
derived masses of these prominences show a scatter of some two orders of
magnitude. In order to investigate if this scatter could be intrinsic, we use a
full magnetic cycle of solar magnetograms to model the coronal structure and
prominence distribution in a young Sun, where we scale the field strength in
the magnetograms with angular velocity according to $ B \propto \Omega^{-1.32}
$. We reproduce both the observed prominence masses and their scatter. We show
that both the field strength and the field geometry contribute to the
prominence masses that can be supported and to the rate at which they are
ejected. Predicted prominence masses follow the magnetic cycle, but with half
the period, peaking both at cycle maximum and at cycle minimum. We show that
mass loss rates in prominences are less than those predicted for the stellar
wind. We also investigate the role of small-scale field that may be unresolved
in typical stellar magnetograms. This provides only a small reduction in the
predicted total prominence mass, principally by reducing the number of large
magnetic loops that can support slingshot prominences. We conclude that the
observed scatter in prominence masses can be explained by underlying magnetic
cycles.
