Although the differences between observed p-mode eigenfrequencies and those calculated from solar models are small, they are significant.
Strong evidence supports the contention that convection is responsible for much of the discrepancy.
I will review an algorithm we have developed, using a method known as adiabatic switching, which allows us to determine the eigenfrequencies of p-modes in complex convective structures. This requirement is equivalent to the familiar WKB approximation and restricts our considerations to large-scale convective motions. Our investigations show that simple models of convective cells produce downshifts which are second-order in the strength of the perturbation. More complex simulations, while consistently displaying downshifts, exhibit more complicated dependences on the strength of the convection. Finally, we demonstrate the dependence of the shift on the radial order n and degree l of the modes and show they agree with analytic estimates.