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The S-stars have been suggested to be a brief transitional phase as starsevolve from oxygen-rich M-type stars into carbon stars, through the dredge upof carbon from He-shell burning. As possible transition objects, S-stars mighthelp achieve a deeper understanding of the chemical evolution as a star ascendsthe AGB, as well as shed more light on the mass-loss mechanism. We haveinitiated a large survey of 40 S-stars to observe line emission in commonmolecules such as CO, SiO, HCN, CS and SiS. Detailed radiative transfermodelling of multi-transition CO radio line observations towards a sample of 40S-stars shows that the mass-loss rate distribution of S-stars is consistentwith those found for M-type AGB stars and carbon stars. Initial results frommodelling of the circumstellar SiO emission are also presented.

The physics and chemistry of circumstellar envelopes of S-stars on the AGB