  Coronal mass ejections (CMEs) are eruptive events that cause a solar-type
star to shed mass and magnetic flux. CMEs tend to occur together with flares,
radio storms, and bursts of energetic particles. On the Sun, CME-related mass
loss is roughly an order of magnitude less intense than that of the background
solar wind. However, on other types of stars, CMEs have been proposed to carry
away much more mass and energy than the time-steady wind. Earlier papers have
used observed correlations between solar CMEs and flare energies, in
combination with stellar flare observations, to estimate stellar CME rates.
This paper sidesteps flares and attempts to calibrate a more fundamental
correlation between surface-averaged magnetic fluxes and CME properties. For
the Sun, there exists a power-law relationship between the magnetic filling
factor and the CME kinetic energy flux, and it is generalized for use on other
stars. An example prediction of the time evolution of wind/CME mass-loss rates
for a solar-mass star is given. A key result is that for ages younger than
about 1 Gyr (i.e., activity levels only slightly higher than the present-day
Sun), the CME mass loss exceeds that of the time-steady wind. At younger ages,
CMEs carry 10 to 100 times more mass than the wind, and such high rates may be
powerful enough to dispel circumstellar disks and affect the habitability of
nearby planets. The cumulative CME mass lost by the young Sun may have been as
much as 1% of a solar mass.
