  Coronal Mass Ejections (CMEs) may have major importance for planetary and
stellar evolution. Stellar CME parameters, such as mass and velocity, have yet
not been determined statistically. So far only a handful of stellar CMEs has
been detected mainly on dMe stars using spectroscopic observations. We
therefore aim for a statistical determination of CMEs of solar-like stars by
using spectroscopic data from the ESO phase 3 and Polarbase archives. To
identify stellar CMEs we use the Doppler signal in optical spectral lines being
a signature of erupting filaments which are closely correlated to CMEs. We
investigate more than 3700 hours of on-source time of in total 425 dF-dK stars.
We find no signatures of CMEs and only few flares. To explain this low level of
activity we derive upper limits for the non detections of CMEs and compare
those with empirically modelled CME rates. To explain the low number of
detected flares we adapt a flare power law derived from EUV data to the
H{\alpha} regime, yielding more realistic results for H{\alpha} observations.
In addition we examine the detectability of flares from the stars by extracting
Sun-as-a-star H{\alpha} light curves. The extrapolated maximum numbers of
observable CMEs are below the observationally determined upper limits, which
indicates that the on-source times were mostly too short to detect stellar CMEs
in H{\alpha}. We conclude that these non detections are related to
observational biases in conjunction with a low level of activity of the
investigated dF-dK stars.
