  We investigate the contribution of very weak flares to the coronal luminosity
of low-mass active stars. We analyze EUVE/DS events data from FK Aqr, V1054
Oph, and AD Leo and conclude that in all these cases the coronal emission is
dominated by flares to such an extent that in some cases the entire emission
may be ascribed to flare heating. We have developed a new method to directly
model for the first time stochastically produced flare emission, including
undetectable flares, and their effects on the observed photon arrival times. We
find that the index of the power-law distribution of flare energies (dN/dE ~
E^{-alpha}) is 2.6+-0.34, 2.74+-0.35, and 2.03-2.32 for FK Aqr, V1054 Oph, and
AD Leo respectively. We also find that the flare component accounts for a large
fraction (generally >50 percent) of the total flux.
