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For distant stars, as observed by the NASA Kepler satellite, parallaxinformation is currently of fairly low quality and is not complete. This limitsthe precision with which the absolute sizes of the stars and their potentialtransiting planets can be determined by traditional methods. Asteroseismologywill be used to aid the radius determination of stars observed during NASA'sKepler mission. We report on the recent asteroFLAG hare-and-hounds Exercise#2,where a group of `hares' simulated data of F-K main-sequence stars that a groupof `hounds' sought to analyze, aimed at determining the stellar radii. Based onthe asteroseismic large frequency spacing, obtained from simulations of 4-yeartime series data from the Kepler mission, we demonstrate that the stellar radiican be correctly and precisely determined, when combined with traditionalstellar parameters from the Kepler Input Catalogue. The radii found by thevarious methods used by each independent hound generally agree with the truevalues of the artificial stars to within 3%, when the large frequency spacingis used. This is 5--10 times better than the results where seismology is notapplied. These results give strong confidence that radius estimation can beperformed to better than 3% for solar-like stars using automatic pipelinereduction. Even when the stellar distance and luminosity are unknown we canobtain the same level of agreement.

Radius determination of solar-type stars using asteroseismology: What to expect from the Kepler mission