  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, here we present stellar wind models for the active
planet-hosting M dwarf AU Mic. Our models incorporate the large-scale
photospheric magnetic field map of the star, reconstructed using the
Zeeman-Doppler Imaging method. We use our models to assess if planet-induced
radio emission could be generated in the corona of AU Mic, through a mechanism
analogous to the sub-Alfv\'enic Jupiter-Io interaction. In the case that AU Mic
has a mass-loss rate of 27 times that of the Sun, we find that both planets b
and c in the system can induce radio emission from 10 MHz to 3 GHz in the
corona of the host star for the majority of their orbits, with peak flux
densities of 10 mJy. Our predicted emission bears a striking similarity to that
recently reported from GJ 1151 by Vedantham et al. (2020), which is indicative
of being induced by a planet. Detection of such radio emission would allow us
to place an upper limit on the mass-loss rate of the star.
