  Asteroseismology of non-radial pulsations in Hot B Subdwarfs (sdB stars)
offers a unique view into the interior of core-helium-burning stars.
Ground-based and space-borne high precision light curves allow for the analysis
of pressure and gravity mode pulsations to probe the structure of sdB stars
deep into the convective core. As such asteroseismological analysis provides an
excellent opportunity to test our understanding of stellar evolution. In light
of the newest constraints from asteroseismology of sdB and red clump stars,
standard approaches of convective mixing in 1D stellar evolution models are
called into question. The problem lies in the current treatment of overshooting
and the entrainment at the convective boundary. Unfortunately no consistent
algorithm of convective mixing exists to solve the problem, introducing
uncertainties to the estimates of stellar ages. Three dimensional simulations
of stellar convection show the natural development of an overshooting region
and a boundary layer. In search for a consistent prescription of convection in
one dimensional stellar evolution models, guidance from three dimensional
simulations and asteroseismological results is indispensable.
