Abstract
We present preliminary results of a study in which we determine the chemical composition of the transferred material in AM CVn systems as a function of the formation channel and progenitor metallicity. Using a detailed stellar evolution code we simulate the formation of the donor star in AM CVn systems and its evolution during the mass transfer. The chemical composition of the outer layers of the donor, and thus of the accretion disc, can used as input for accretion disc models, and subsequently compared to observed AM CVn spectra.
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