  We explore the ramification of associating the energetics of extreme mag-
netic reconnection events with transient mass loss in a stellar analogy with
solar eruptive events. We establish energy partitions relative to the total
bolometric radiated flare energy for different observed components of stellar
flares, and show that there is rough agreement for these values with solar
flares. We apply an equipartition between the bolometric radiated flare energy
and kinetic energy in an accompanying mass ejection, seen in solar eruptive
events and expected from reconnection. This allows an integrated flare rate in
a particular waveband to be used to estimate the amount of associated transient
mass loss. This approach is supported by a good correspondence between
observational flare signatures on high flaring rate stars and the Sun, which
suggests a common physical origin. If the frequent and extreme flares that
young solar-like stars and low-mass stars experience are accompanied by
transient mass loss in the form of coronal mass ejections, then the cumulative
effect of this mass loss could be large. We find that for young solar-like
stars and active M dwarfs, the total mass lost due to transient magnetic
eruptions could have significant impacts on disk evolution, and thus planet
formation, and also exoplanet habitability.
