  The eclipsing binary CM Dra contains nearly identical red dwarfs of spectral
class dM4.5. Their masses and radii have been reported with unprecedentedly
small statistical errors. When compared with standard stellar models of
appropriate age (\approx4 Gyr), the empirical results indicate that both
components are larger in R, and lower in luminosity L, by several standard
deviations. Here, we attempt at first to model the components in the context of
standard stellar models using differ
