  Most current models of low mass red giant stars do not reproduce the observed
position of the red giant branch luminosity bump, a diagnostic of the maximum
extent of the convective envelope during the first dredge up. Global
asteroseismic parameters, the large frequency separation and frequency of
maximum oscillation power, measured for large samples of red giants, show that
modeling convective overshoot below the convective envelope helps match the
modeled luminosity bump positions to observations. However, these global
parameters cannot be used to probe envelope overshoot in a star-by-star manner.
Red giant mixed modes, which behave like acoustic modes at the surface and like
gravity modes in the core, contain important information about the interior
structure of the star, especially near the convective boundary. Therefore,
these modes may be used to probe interior processes, such as overshoot. Using a
grid of red giant models with varying mass, metallicity, surface gravity,
overshoot treatment, and amount of envelope overshoot, we find that changing
the overshoot amplitude (and prescription) of overshoot below the convection
zone in red giant stellar models results in significant differences in the
evolution of the models' dipole mixed-mode oscillation frequencies, the average
mixed mode period spacing, $\langle \Delta P \rangle$, and gravity mode phase
offset term, $\epsilon_g$.
