  Recent numerical simulations by Freytag et al. of the outer convection
envelope of the cool super-giant Betelgeuse, have shown that the fluctuations
in the star's apparent luminosity may be caused by giant cell convection. These
simulations bring forth the possibility of addressing another question; namely
whether stars such as Betelgeuse may harbor magnetic activity. Taking the
detailed numerical simulations of the star at face value, we have applied a
kinematic dynamo analysis, to study whether the flow field of the super-giant
may be able to amplify a weak seed magnetic field. We do indeed find a positive
exponential growth rate of the magnetic energy. The possible Betelgeusian
dynamo may be characterized as belonging to the class of so-called ``local
small-scale dynamos'' (i.e. dynamos where rotation is not dominant), but this
is a less meaningful designation in the case of Betelgeuse, since the field is
both global and large-scale.
