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-Alfvénic Jupiter-Io interaction. In the case that AU Mic has a mass-loss rate of < 590 times that of the Sun, we find that both planets b and c in the system can induce radio emission from 10 MHz – 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.

{"references": ["van der Holst, Bart et al. (2014). Alfv\u00e9n Wave Solar Model (AWSoM): Coronal Heating.", "Klein, Baptiste et al. (2021b). Investigating the young AU Mic system with SPIRou: large-scale stellar magnetic field and close-in planet mass.", "Turnpenney, Sam et al. (2018). Exoplanet-induced Radio Emission from M Dwarfs.", "Vedantham, Harish et al (2020). Coherent radio emission from a quiescent red dwarf indicative of star-planet interaction."]}