  We assess the potential of asteroseismology for determining the fundamental
properties of individual $\delta$ Scuti stars. We computed a grid of evolution
and adiabatic pulsation models using the Yale Rotating Evolution Code to study
the systematic changes in low-order ($\ell = 0, 1, 2,$ and 3) modes as
functions of fundamental stellar properties. Changes to the stellar mass,
chemical composition, and convective core overshooting length change the
observable pulsation spectrum significantly. In general, mass has the strongest
effect on evolution and on pulsation, followed by the metal abundance. Changes
to the helium content have very little effect on the frequencies until near the
end of the main sequence. Changes to each of the four parameters change the
$p$-mode frequencies more, both in absolute and relative terms, than they do
the $g$- and mixed-mode frequencies, suggesting that these parameters have a
greater effect on the outer layers of the star.
  We also present evolution and pulsation models of the well-studied star FG
Virginis, outlining a possible method of locating favorable models in the
stellar parameter space based upon a definitive identification of only two
modes. Specifically, we plot evolution models on the (period-period ratio) and
(temperature-period ratio) planes to select candidate models, and modify the
core overshooting parameter to fit the observed star. For these tests, we
adjusted only the mass, helium and metal abundances, and core overshooting
parameter, but this method can be extended to include the effects of
first-order rotational splitting and second-order rotational distortion of
pulsation spectra.
