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Asteroseismic measurements enable inferences of the underlying stellarstructure, such as the density and the speed of sound at various points withinthe interior of the star. This provides an opportunity to test stellarevolution theory by assessing whether the predicted structure of a star agreeswith the measured structure. Thus far, this kind of inverse analysis has onlybeen applied to the Sun and three solar-like main-sequence stars. Here weextend the technique to stars on the subgiant branch, and apply it to one ofthe best-characterized subgiants of the Kepler mission, HR 7322. Theobservation of mixed oscillation modes in this star facilitates inferences ofthe conditions of its inert helium core, nuclear-burning hydrogen shell, andthe deeper parts of its radiative envelope. We find that despite significantdifferences in the mode frequencies, the structure near to the center of thisstar does not differ significantly from the predicted structure.

Asteroseismic Inference of the Central Structure in a Subgiant Star