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Asteroseismology of Hot B Subdwarfs (sdB stars) provides insight into the interior of core-helium-burning stars, testing stellar evolution understanding. Standard 1D stellar evolution models' convective mixing approaches are questioned due to inconsistencies with asteroseismological results, particularly regarding overshooting and convective boundary entrainment. Three-dimensional simulations and asteroseismology guidance are necessary to develop a consistent convection prescription. sdB stars, with thin hydrogen envelopes and helium-burning cores, exhibit non-radial pulsations, including pressure (p-) and gravity (g-) modes, which probe the star's structure, especially the convective core and chemical transitions. Asteroseismological analysis of g-mode pulsators offers a unique window into the interior of core helium-burning stars, allowing for quantitative studies of their structure and evolution.