Low-mass eclipsing binaries show systematically larger radii than model predictions for their mass , metallicity and age .
Prominent explanations for the inflation involve enhanced magnetic fields generated by rapid rotation of the star that inhibit convection and/or suppress flux from the star via starspots .
However , derived masses and radii for individual eclipsing binary systems often disagree in the literature .
In this paper , we continue to investigate low-mass eclipsing binaries ( EBs ) observed by NASA ’ s Kepler spacecraft , deriving stellar masses and radii using high-quality space-based light curves and radial velocities from high-resolution infrared spectroscopy .
We report masses and radii for three Kepler EBs , two of which agree with previously published masses and radii ( KIC 11922782 and KIC 9821078 ) .
For the third EB ( KIC 7605600 ) , we report new masses and show the secondary component is likely fully convective ( M _ { 2 } = 0.17 \pm 0.01 M _ { \sun } and R _ { 2 } = 0.199 ^ { +0.001 } _ { -0.002 } R _ { \sun } ) .
Combined with KIC 10935310 from Han et al .
( 2017 ) , we find that the masses and radii for four low-mass Kepler EBs are consistent with modern stellar evolutionary models for M dwarf stars and do not require inhibited convection by magnetic fields to account for the stellar radii .