  We describe an approach for finding the eigenfrequencies of solar acoustic
modes (p modes) in a convective envelope in the WKB limit. This approximation
restricts us to examining the effects of fluid motions which are large compared
to the mode wavelength, but allows us to treat the three-dimensional mode as a
localized ray. The method of adiabatic switching is then used to investigate
the frequency shifts resulting from simple perturbations to a polytropic model
of the convection zone as well as from two basic models of a convective cell.
We find that although solely depth-dependent perturbations can give frequency
shifts which are first order in the strength of the perturbation, models of
convective cells generate downward frequency shifts which are second order in
the perturbation strength. These results may have implications for resolving
the differences between eigenfrequencies derived from solar models and those
found from helioseismic observations.
