  Observations indicate that magnetic fields in rapidly rotating stars are very
strong, on both small and large scales. What is the nature of the resulting
corona? Here we seek to shed some light on this question. We use the results of
an anelastic dynamo simulation of a rapidly rotating fully-convective M-star to
drive a physics-based model for the stellar corona. We find that due to the
several kilo Gauss large-scale magnetic fields at high latitudes, the corona
and its X-ray emission are dominated by star-size large hot loops, while the
smaller, underlying colder loops are not visible much in the X-ray. Based on
this result we propose that, in rapidly rotating stars, emission from such
coronal structures dominates the quiescent, cooler but saturated X-ray
emission.
