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Main sequence, fully-convective M dwarfs in eclipsing binaries are observedto be larger than stellar evolutionary models predict by as much as $10-15\%$.A proposed explanation for this discrepancy involves effects from strongmagnetic fields, induced by rapid-rotation via the dynamo process. Although, ahandful of single, slowly-rotating M dwarfs with radius measurements frominterferometry also appear to be larger than models predict, suggesting thatrotation or binarity specifically may not be the sole cause of the discrepancy.We test whether single, rapidly rotating, fully convective stars are alsolarger than expected by measuring their $R \sin i$ distribution. We combinephotometric rotation periods from the literature with rotational broadening ($v\sin i$) measurements reported in this work for a sample of 88 rapidly rotatingM dwarf stars. Using a Bayesian framework, we find that stellar evolutionarymodels underestimate the radii by $10-15\% \substack{+3 \\ -2.5}$, but that athigher masses ($0.18<M<0.4 M_{Sun}$) the discrepancy is only about $6\%$ andcomparable to results from interferometry and eclipsing binaries. At the lowestmasses ($0.08<M<0.18 M_{Sun}$), we find the discrepancy between observationsand theory is $13-18\%$, and we argue that the discrepancy is unlikely to bedue to effects from age. Furthermore, we find no statistically significantradius discrepancy between our sample and the handful of M dwarfs withinterferometric radii. We conclude that neither rotation nor binarity isresponsible for the inflated radii of fully convective M dwarfs, and that allfully-convective M dwarfs are larger than models predict.

Magnetic Inflation and Stellar Mass II: On the Radii of Single, Rapidly Rotating, Fully Convective M Dwarf Stars