Constraining stellar CMEs

A lot has been done on an observational basis in the past with respect to stellar coronal mass ejections. Using the method of Doppler-shifted emission/absorption, still, only fast events can be unambiguously identified with erupting filaments/prominences. These often form the cores of CMEs on the Sun. From dM stars we know that there are numerous observations of Doppler-shifted emission events with projected velocities of 100-300km/s.
Constraints are needed to better interpret those signatures which are potential CME candidates. We have chosen cloud modeling to constrain what might produce such signatures. We focus on one known event from the literature, found on the fast rotating dMe star V374 Peg, and find that both a filament and a prominence scenario reproduces the peak flux of the Doppler-shifted emission signatures, contrary to the solar case where filaments produce an absorption signature in the Balmer lines. The deduced parameters from modeling show values in the upper range of solar prominence parameters, except engfor temperature and area, which are larger. A prominence/filament eruption scenario is therefore very likely for the event found on V374 Peg.