  MQ Dra is a strongly magnetic Cataclysmic Variable whose white dwarf accretes
material from its secondary star through a stellar wind at a low rate. TESS
observations were made of MQ Dra in four sectors in Cycle 2 and show a short
duration, high energy flare (~10^35 erg) which has a profile characteristic of
a flare from the M5V secondary star. This is one of the few occasions where an
energetic flare has been seen from a Polar. We find no evidence that the flare
caused a change in the light curve following the event and consider whether a
coronal mass ejection was associated with the flare. We compare the frequency
of energetic flares from the secondary star in MQ Dra with M dwarf stars and
discuss the overall flare rate of stars with rotation periods shorter than 0.2
d and how such fast rotators can generate magnetic fields with low differential
rotation rates.
