Computations of a White Dwarf model Grid for Studies in Astroseismology

White dwarf stars are the final evolutionary stage of ~95% of all single stars that are born in the universe. Therefore, learning about these stars is extremely important as they place necessary constraints on stellar evolution as a whole. The only way to probe stellar interiors is through asteroseismology, which consists of comparing the observed pulsation periods to models. We computed a model grid using the Modules for Experiments in Stellar Astrophysics (MESA), an open-source 1D stellar evolution code, and the theoretical modes using Gyre. We have done asteroseismology determinations for a few white dwarf stars, determining the photospheric parameters, as well as mass and internal composition. Furthermore, to determine the external uncertainties, we have compared our results to the asteroseismology using other codes, such as the White Dwarf Evolutionary Code (WDEC). Our results are very relevant to validate the state-of-the-art asteroseismological models.