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Eclipsing binaries with M-type components are still rare objects. Strongobservational biases have made that today only a few eclipsing binaries withcomponent masses below 0.6 Msun and well-determined fundamental properties areknown. However, even in these small numbers the detailed comparison of theobserved masses and radii with theoretical predictions has revealed largedisagreements. Current models seem to predict radii of stars in the 0.4-0.8Msun range to be some 5-15% smaller than observed. Given the high accuracy ofthe empirical measurements (a few percent in both mass and radius), thesedifferences are highly significant. I review all the observational evidence onthe properties of M-type stars and discuss a possible scenario based on stellaractivity to explain the observed discrepancies.Comment: 8 pages, 1 figure, proceedings of the meeting "Close Binaries in the  21st Century

Masses and Radii of Low-Mass Stars: Theory Versus Observations