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Several low-mass eclipsing binary stars show larger than expected radii fortheir measured mass, metallicity and age. One proposed mechanism for thisradius inflation involves inhibited internal convection and starspots caused bystrong magnetic fields. One particular eclipsing binary, T-Cyg1-12664, hasproven confounding to this scenario. \citet{Cakirli2013a} measured a radius forthe secondary component that is twice as large as model predictions for starswith the same mass and age, but a primary mass that is consistent withpredictions. \citet[][]{Iglesias2017} independently measured the radii andmasses of the component stars and found that the radius of the secondary is notin fact inflated with respect to models, but that the primary is, consistentwith the inhibited convection scenario. However, in their mass determinations,\citet[][]{Iglesias2017} lacked independent radial velocity measurements forthe secondary component due to the star's faintness at optical wavelengths. Thesecondary component is especially interesting as its purported mass is near thetransition from partially-convective to a fully-convective interior. In thisarticle we independently determined the masses and radii of the component starsof T-Cyg1-12664 using archival {\it Kepler} data and radial velocitymeasurements of both component stars obtained with IGRINS on the DiscoveryChannel Telescope and NIRSPEC and HIRES on the Keck Telescopes. We show thatneither of the component stars is inflated with respect to models. Our resultsare broadly consistent with modern stellar evolutionary models formain-sequence M dwarf stars and do not require inhibited convection by magneticfields to account for the stellar radii.

Magnetic Inflation and Stellar Mass I: Revised Parameters for the Component Stars of the Kepler Low-mass Eclipsing Binary T-Cyg1-12664