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