Light Curve Modeling of Eclipsing Binary Systems with Delta Scuti Component

Abstract

Astroseismology in eclipsing binaries with Delta ($\delta$) Scuti components offers a powerful means to derive stellar parameters and probe internal structures. To enable accurate frequency analysis, binary characteristics must be disentangled from the observed light curves. This study utilizes the LC2015 light curve modeling method, followed by the DC2015 differential correction process, integrated into the Wilson-Devinney (WD) eclipsing binary modeling code. The analysis focuses on two $\delta$ Scuti binary systems, KIC 8504570 and SX DRACONIS (Dra), using Kepler and TESS photometric data, supplemented by literature-derived initial stellar parameters. The DC2015 process employs the Levenberg-Marquardt algorithm to minimize the difference between observed and modeled light curves. The refined models provide highly accurate stellar parameters, including primary and secondary star temperatures ($T_{eff},1$ and $T_{eff},2$), mass ratio (q), and primary star luminosity (L1) with associated errors. For KIC 8504570: $T_{eff},1$ (7400.9 $\pm$ 1.6) K, $T_{eff},2$ (5450.0 $\pm$ 1.0) K, q (0.5208 $\pm$ 0.0002), and L1 (11.8043 $\pm$ 0.0006)$L_\odot$. For SX Dra: $T_{eff},1$ (7729.7 $\pm$ 1.1) K , $T_{eff},2$ (4927.5 $\pm$ 0.5) K, q (0.4772 $\pm$ 0.0006), and L1 (7.0474 $\pm$ 0.0015)$L_\odot$.