  Many low-mass pre-main-sequence stars exhibit strong magnetic activity and
coronal X-ray emission. Even after the primordial accretion disk has been
cleared out, the star's high-energy radiation continues to affect the formation
and evolution of dust, planetesimals, and large planets. Young stars with
debris disks are thus ideal environments for studying the earliest stages of
non-accretion-driven coronae. In this paper we simulate the corona of AU Mic, a
nearby active M dwarf with an edge-on debris disk. We apply a self-consistent
model of coronal loop heating that was derived from numerical simulations of
solar field-line tangling and magnetohydrodynamic turbulence. We also
synthesize the modeled star's X-ray luminosity and thermal radio/millimeter
continuum emission. A realistic set of parameter choices for AU Mic produces
simulated observations that agree with all existing measurements and upper
limits. This coronal model thus represents an alternative explanation for a
recently discovered ALMA central emission peak that was suggested to be the
result of an inner "asteroid belt" within 3 AU of the star. However, it is also
possible that the central 1.3 mm peak is caused by a combination of active
coronal emission and a bright inner source of dusty debris. Additional
observations of this source's spatial extent and spectral energy distribution
at millimeter and radio wavelengths will better constrain the relative
contributions of the proposed mechanisms.
