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Magnetic fields are hypothesized to inflate the radii of low-massstars---defined as less massive than 0.8$M_\odot$---in detached eclipsingbinaries (DEBs). We investigate this hypothesis using the recently introducedmagnetic Dartmouth stellar evolution code. In particular, we focus on starsthought to have a radiative core and convective outer envelope by studying indetail three individual DEBs: UV Psc, YY Gem, and CU Cnc. The results suggestthat the stabilization of thermal convection by a magnetic field is a plausibleexplanation for the observed model-radius discrepancies. However, surfacemagnetic field strengths required by the models are significantly stronger thanthose estimated from the observed coronal X-ray emission. Agreement betweenmodel predicted surface magnetic field strengths and those inferred from X-rayobservations can be found by assuming that the magnetic field sources itsenergy from convection. This approach makes the transport of heat by convectionless efficient and is akin to reduced convective mixing length methods used inother studies. Predictions for the metallicity and magnetic field strengths ofthe aforementioned systems are reported. We also develop an expression relatinga reduction in the convective mixing length to a magnetic field strength inunits of the equipartition value. Our results are compared with those fromprevious investigations to incorporate magnetic fields to explain the low-massDEB radius inflation. Finally, we explore how the effects of magnetic fieldsmight affect mass determinations using asteroseismic data and the implicationof magnetic fields on exoplanet studies.

Magnetic Inhibition of Convection and the Fundamental Properties of Low-Mass Stars. I. Stars with a Radiative Core