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There are strong observational indications that the dense slow winds of coolluminous AGB stars are driven by radiative pressure on dust grains which formin the extended atmospheres resulting from pulsation-induced shocks. For carbonstars, detailed models of outflows driven by amorphous carbon grains show goodagreement with observations. Some still existing discrepancies may be due to asimplified treatment of cooling in shocks, drift of the grains relative to thegas, or effects of giant convection cells or dust-induced pattern formation.For stars with C/O < 1, recent models indicate that absorption by silicate dustis probably insuffcient to drive their winds. A possible alternative isscattering by Fe-free silicate grains with radii of a few tenths of a micron.In this scenario one should expect less circumstellar reddening for M- andS-type AGB stars than for C-stars with comparable stellar parameters and massloss rates.

Starlight and Sandstorms: Mass Loss Mechanisms on the AGB