  We investigate the pulsational properties of RSG models --- which we evolve
from ZAMS masses in the range 10 to $20 \Msun$ --- by means of linear and
non-linear calculations. We find period and growth rate of the dominant
fundamental mode to increase with increasing luminosity-to-mass ratio $L/M$.
Our models obtain relatively large $L/M$ values due to the inclusion of
rotation in the evolutionary calculations; however, the largest values are
obtained at and beyond central He-exhaustion due to major internal
rearrangements of the nuclear burning regions. Our non-linear calculations as
well as the behavior of the linear period and growth rate of the pulsations for
periods approaching the Kelvin-Helmholtz time scale of the H-rich stellar
envelope point towards the possibility of large amplitude pulsations. Such
properties are similar to that found in AGB stars and suggest the possibility
of a ``superwind'' to occur before the RSGs explode as supernovae. We conclude
that changes in global stellar properties during the last few $10^4 \yr$ before
core collapse may lead to drastic changes in the pulsational and wind
properties of pre-supernova stars, with marked consequences for the immediate
pre-supernova structure of the star and the circumstellar medium. We compare
our results with observations of long-period OH/IR variables and discuss
observational evidence for our scenario from observed supernova light curves,
spectra and remnants.
