  Planets that closely orbit magnetically active stars are thought to be able
to interact with their magnetic fields in a way that modulates stellar
activity. This modulation in phase with the planetary orbit, such as enhanced
X-ray activity, chromospheric spots, radio emission, or flares, is considered
the clearest sign of magnetic star-planet interaction (SPI). However, the
magnitude of this interaction is poorly constrained, and the intermittent
nature of the interaction is a challenge for observers. AU Mic is an early M
dwarf, and the most actively flaring planet host detected to date. Its
innermost companion, AU Mic b, is a promising target for magnetic SPI
observations. We used optical light curves of AU Mic obtained by the Transiting
Exoplanet Survey Satellite to search for signs of flaring SPI with AU Mic b
using a customized Anderson-Darling test. In the about $50$ days of
observations, the flare distributions with orbital, rotational, and synodic
periods were generally consistent with intrinsic stellar flaring. We found the
strongest deviation ($p=0.07,\;n=71$) from intrinsic flaring with the orbital
period of AU Mic b, in the high energy half of our sample ($ED>1$ s). If it
reflects the true SPI signal from AU Mic b, extending the observing time by a
factor of $2-3$ will yield a $>3\sigma$ detection. Continued monitoring of AU
Mic may therefore reveal flaring SPI with orbital phase, while rotational
modulation will smear out due to the star's strong differential rotation.
