  There have recently been detections of radio emission from low-mass stars,
some of which are indicative of star-planet interactions. Motivated by these
exciting new results, in this paper we present Alfv\'en wave-driven stellar
wind models of the two active planet-hosting M dwarfs Prox Cen and AU Mic. Our
models incorporate large-scale photospheric magnetic field maps reconstructed
using the Zeeman-Doppler Imaging method. We obtain a mass-loss rate of
$0.25~\dot{M}_{\odot}$ for the wind of Prox Cen. For the young dwarf AU Mic, we
explore two cases: a low and high mass-loss rate. Depending on the properties
of the Alfv\'en waves which heat the corona in our wind models, we obtain
mass-loss rates of $27$ and $590~\dot{M}_{\odot}$ for AU Mic. We use our
stellar wind models to assess the generation of electron cyclotron maser
instability emission in both systems, through a mechanism analogous to the
sub-Alfv\'enic Jupiter-Io interaction. For Prox Cen we do not find any feasible
scenario where the planet can induce radio emission in the star's corona, as
the planet orbits too far from the star in the super-Alfv\'enic regime.
However, in the case that AU Mic has a stellar wind mass-loss rate of
$27~\dot{M}_{\odot}$, we find that both planets b and c in the system can
induce radio emission from $\sim10$ MHz to 3 GHz in the corona of the host star
for the majority of their orbits, with peak flux densities of $\sim10$ mJy.
Detection of such radio emission would allow us to place an upper limit on the
mass-loss rate of the star.
