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The goal of stellar evolution theory is to predict the structure of starsthroughout their lifetimes. Usually, these predictions can be assessed onlyindirectly, for example by comparing predicted and observed effectivetemperatures and luminosities. Thanks now to asteroseismology, which can revealthe internal structure of stars, it becomes possible to compare the predictionsfrom stellar evolution theory to actual stellar structures. In this work, wepresent an inverse analysis of the oscillation data from the solar-type starKIC 6225718, which was observed by the \emph{Kepler} space observatory duringits nominal mission. As its mass is about 20% greater than solar, this star ispredicted to transport energy by convection in its nuclear-burning core. Wefind significant differences between the predicted and actual structure of thestar in the radiative interior near to the convective core. In particular, thepredicted sound speed is higher than observed in the deep interior of the star,and too low at a fractional radius of 0.25 and beyond. The cause of thesediscrepancies is unknown, and is not remedied by known physics in the form ofconvective overshooting or elemental diffusion.

Testing stellar evolution with asteroseismic inversions of a main sequence star harboring a small convective core