  Conventional astrophysical observations have failed to provide stringent
constraints on physical processes operating in the interior of the stars.
However, satellite missions now promise a solution to these problems by
providing long-term high-quality continuous data which will allow the
application of seismic techniques. With this in mind, and using the Sun as our
astrophysical laboratory, our aim is to determine if Corot- and Kepler-like
asteroseismic data can constrain physical processes like microscopic diffusion.
We test to what extent can the observed atmospheric abundances coupled with
p-mode frequencies safely distinguish between stellar initial chemical
composition and diffusion of these elements. We present some preliminary
results of our analysis.
