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Most extrasolar planets have been detected by their influence on their parentstar, typically either gravitationally (the Doppler method) or by the small dipin brightness as the planet blocks a portion of the star (the transit method).Therefore, the accuracy with which we know the masses and radii of extrasolarplanets depends directly on how well we know those of the stars, the latterusually determined from the measured stellar surface gravity, logg. Recent workhas demonstrated that the short-timescale brightness variations ("flicker") ofstars can be used to measure logg to a high accuracy of ~0.1-0.2 dex (Bastienet al. 2013). Here, we use flicker measurements of 289 bright (Kepmag<13)candidate planet-hosting stars with Teff=4500-6650 K to re-assess the stellarparameters and determine the resulting impact on derived planet properties.This re-assessment reveals that for the brightest planet-host stars, anastrophysical bias exists that contaminates the stellar sample with evolvedstars: nearly 50% of the bright planet-host stars are subgiants. As a result,the stellar radii, and hence the radii of the planets orbiting these stars, areon average 20-30% larger than previous measurements had suggested.

Larger Planet Radii Inferred from Stellar "Flicker" Brightness Variations of Bright Planet Host Stars