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Empirically, the X-ray luminosity LX from M dwarfs has been found to have anupper limit of about 0.2% of the bolometric flux Lbol. In the limit wheremagnetic fields in M dwarfs are generated in equipartition with convectivemotions, we use stellar models to calculate the energy flux of Alfven waves FAas a function of depth in the sub-surface convection zone. Since Alfven waveshave the optimal opportunity for wave modes to reach the corona, we suggestthat FA sets an upper limit on the mechanical flux Fmech which causes coronalheating. This suggestion accounts quantitatively for the saturated values ofLX/Lbol which have been reported empirically for M dwarfs.

Mechanical energy fluxes associated with saturated coronal heating in M dwarfs: comparison with predictions of a turbulent dynamo