  We examine the hypothesis that magnetic fields are inflating the radii of
fully convective main sequence stars in detached eclipsing binaries (DEBs). The
magnetic Dartmouth stellar evolution code is used to analyze two systems in
particular: Kepler-16 and CM Draconis. Magneto-convection is treated assuming
stabilization of convection and also by assuming reductions in convective
efficiency due to a turbulent dynamo. We find that magnetic stellar models are
unable to reproduce the properties of inflated fully convective main sequence
stars, unless strong interior magnetic fields in excess of 10 MG are present.
Validation of the magnetic field hypothesis given the current generation of
magnetic stellar evolution models therefore depends critically on whether the
generation and maintenance of strong interior magnetic fields is physically
possible. An examination of this requirement is provided. Additionally, an
analysis of previous studies invoking the influence of star spots is presented
to assess the suggestion that star spots are inflating stars and biasing light
curve analyses toward larger radii. From our analysis, we find that there is
not yet sufficient evidence to definitively support the hypothesis that
magnetic fields are responsible for the observed inflation among fully
convective main sequence stars in DEBs.
