  Asteroseismology gives us the opportunity to look inside stars and determine
their internal properties. Based on these observations, estimations can be made
for the amount of the convective boundary mixing and envelope mixing of such
stars, and the shape of the mixing profile in the envelope. However, these
results are not typically included in stellar evolution models. We aim to
investigate the impact of varying convective boundary mixing and envelope
mixing in a range based on asteroseismic modelling in stellar models, both for
the stellar structure and for the nucleosynthetic yields. In this first study,
we focus on the pre-explosive evolution of a 20Msun star and evolve the models
to the final phases of carbon burning. We vary the convective boundary mixing,
implemented as step-overshoot, with the overshoot parameter in the range
0.05-0.4 and the amount of envelope mixing in the range 1-10$^{6}$ with a
mixing profile based on internal gravity waves. We use a large nuclear network
of 212 isotopes to study the nucleosynthesis. We find that enhanced mixing
according to asteroseismology of main-sequence stars, both at the convective
core boundary and in the envelope, has significant effects on the
nucleosynthetic wind yields. Our evolutionary models beyond the main sequence
diverge in yields from models based on rotational mixing, having longer helium
burning lifetimes and lighter helium-depleted cores. We find that the
asteroseismic ranges of internal mixing calibrated from core hydrogen burning
stars lead to similar wind yields as those resulting from the theory of
rotational mixing. Adopting the seismic mixing levels beyond the main sequence,
we find earlier transitions to radiative carbon burning compared to models
based on rotational mixing. This influences the compactness and the occurrence
of shell-mergers, which may affect the supernova properties and explosive
nucleosynthesis.
