Asteroseismology of δ Scuti Stars: A Parameter Study and Application to Seismology of FG Virginis

Abstract

We assess the potential of asteroseismology for determining the fundamental properties of individual δ 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 (l = 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, in both 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 on 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.