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A long-standing issue in the theory of low mass stars is the discrepancybetween predicted and observed radii and effective temperatures. In spite ofthe increasing availability of very precise radius determinations fromeclipsing binaries and interferometric measurements of radii of single stars,there is no unanimous consensus on the extent (or even the existence) of thediscrepancy and on its connection with other stellar properties (e.g.metallicity, magnetic activity). We investigate the radius discrepancyphenomenon using the best data currently available (accuracy about 5%). We haveconstructed a grid of stellar models covering the entire range of low massstars (0.1-1.25 M_sun) and various choices of the metallicity and of the mixinglength parameter \alpha. We used an improved version of the Yale Rotationalstellar Evolution Code (YREC), implementing surface boundary conditions basedon the most up-to-date PHOENIX atmosphere models. Our models are in goodagreement with others in the literature and improve and extend the low mass endof the Yale-Yonsei isochrones. Our calculations include rotation-relatedquantities, such as moments of inertia and convective turnover time scales,useful in studies of magnetic activity and rotational evolution of solar-likestars. Consistently with previous works, we find that both binaries and singlestars have radii inflated by about 3% with respect to the theoretical models;among binaries, the components of short orbital period systems are found to bethe most deviant. We conclude that both binaries and single stars arecomparably affected by the radius discrepancy phenomenon.

The radius discrepancy in low mass stars: single vs. binaries