  The detection of mixed oscillation modes offers a unique insight into the
internal structure of core helium burning (CHeB) stars. The stellar structure
during CHeB is very uncertain because the growth of the convective core, and/or
the development of a semiconvection zone, is critically dependent on the
treatment of convective boundaries. In this study we calculate a suite of
stellar structure models and their non-radial pulsations to investigate why the
predicted asymptotic g-mode $\ell = 1$ period spacing $\Delta\Pi_1$ is
systematically lower than is inferred from Kepler field stars. We find that
only models with large convective cores, such as those calculated with our
newly proposed "maximal-overshoot" scheme, can match the average $\Delta\Pi_1$
reported. However, we also find another possible solution that is related to
the method used to determine $\Delta\Pi_1$: mode trapping can raise the
observationally inferred $\Delta\Pi_1$ well above its true value. Even after
accounting for these two proposed resolutions to the discrepancy in average
$\Delta\Pi_1$, models still predict more CHeB stars with low $\Delta\Pi_1$ ($ <
270$ s) than are observed. We establish two possible remedies for this: i)
there may be a difficulty in determining $\Delta\Pi_1$ for early CHeB stars
(when $\Delta\Pi_1$ is lowest) because of the effect that the sharp composition
profile at the hydrogen burning shell has on the pulsations, or ii) the mass of
the helium core at the flash is higher than predicted. Our conclusions
highlight the need for the reporting of selection effects in asteroseismic
population studies in order to safely use this information to constrain stellar
evolution theory.
