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We examine the hypothesis that magnetic fields are inflating the radii offully convective main sequence stars in detached eclipsing binaries (DEBs). Themagnetic Dartmouth stellar evolution code is used to analyze two systems inparticular: Kepler-16 and CM Draconis. Magneto-convection is treated assumingstabilization of convection and also by assuming reductions in convectiveefficiency due to a turbulent dynamo. We find that magnetic stellar models areunable to reproduce the properties of inflated fully convective main sequencestars, unless strong interior magnetic fields in excess of 10 MG are present.Validation of the magnetic field hypothesis given the current generation ofmagnetic stellar evolution models therefore depends critically on whether thegeneration and maintenance of strong interior magnetic fields is physicallypossible. An examination of this requirement is provided. Additionally, ananalysis of previous studies invoking the influence of star spots is presentedto assess the suggestion that star spots are inflating stars and biasing lightcurve analyses toward larger radii. From our analysis, we find that there isnot yet sufficient evidence to definitively support the hypothesis thatmagnetic fields are responsible for the observed inflation among fullyconvective main sequence stars in DEBs.

Magnetic Inhibition of Convection and the Fundamental Properties of Low-Mass Stars. II. Fully Convective Main Sequence Stars