  The overstability of the fundamental radial mode in M dwarf models was
theoretically predicted by Rodr\'iguez-L\'opez et al. (2012). The periods were
found to be in the ranges ~25-40 min and ~4-8 h, depending on stellar age and
excitation mechanism. We have extended our initial M dwarf model grid in mass,
metallicity, and mixing length parameter. We have also considered models with
boundary conditions from PHOENIX NextGen atmospheres to test their influence on
the pulsation spectra. We find instability of non-radial modes with radial
orders up to k=3, degree l=0-3, including p and g modes, with the period range
extending from 20 min up to 11 h. Furthermore, we find theoretical evidence of
the potential of M dwarfs as solar-like oscillators.
