  Solar CMEs and flares have a statistically well defined relation, with more
energetic X-ray flares corresponding to faster and more massive CMEs. How this
relation extends to more magnetically active stars is a subject of open
research. Here, we study the most probable stellar CME candidates associated
with flares captured in the literature to date, all of which were observed on
magnetically active stars. We use a simple CME model to derive masses and
kinetic energies from observed quantities, and transform associated flare data
to the GOES 1--8~\AA\ band. Derived CME masses range from $\sim 10^{15}$ to
$10^{22}$~g. Associated flare X-ray energies range from $10^{31}$ to
$10^{37}$~erg. Stellar CME masses as a function of associated flare energy
generally lie along or below the extrapolated mean for solar events. In
contrast, CME kinetic energies lie below the analogous solar extrapolation by
roughly two orders of magnitude, indicating approximate parity between flare
X-ray and CME kinetic energies. These results suggest that the CMEs associated
with very energetic flares on active stars are more limited in terms of the
ejecta velocity than the ejecta mass, possibly because of the restraining
influence of strong overlying magnetic fields and stellar wind drag. Lower CME
kinetic energies and velocities present a more optimistic scenario for the
effects of CME impacts on exoplanets in close proximity to active stellar
hosts.
