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We present empirical relations for determining the amount by which theeffective temperatures and radii---and therefore the estimated masses---oflow-mass stars and brown dwarfs are altered due to chromospheric activity.Accurate estimates of stellar radii are especially important in the context ofsearches for transiting exoplanets, which rely upon the assumed stellarradius/density to infer the planet radius/density. Our relations are based on alarge set of well studied low-mass stars in the field and on a set of benchmarklow-mass eclipsing binaries. The relations link the amount by which an activeobject's temperature is suppressed, and its radius inflated, to the strength ofits Halpha emission. These relations are found to approximately preservebolometric luminosity. We apply these relations to the peculiar brown-dwarfeclipsing binary 2M0535-05, in which the active, higher-mass brown dwarf has acooler temperature than its inactive, lower-mass companion. The relationscorrectly reproduce the observed temperatures and radii of 2M0535-05 afteraccounting for the Halpha emission; 2M0535-05 would be in precise agreementwith theoretical isochrones were it inactive. The relations that we present areapplicable to brown dwarfs and low-mass stars with masses below 0.8 Msun andfor which the activity, as measured by Halpha, is in the range -4.6 < logLha/Lbol < -3.3. We expect these relations to be most useful for correctingradius and mass estimates of low-mass stars and brown dwarfs over their activelifetimes (few Gyr). We also discuss the implications of this work fordeterminations of young cluster IMFs.

Correcting for Activity Effects on the Temperatures, Radii, and Estimated Masses of Low-Mass Stars and Brown Dwarfs