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Stellar winds of cool and pulsating asymptotic giant branch (AGB) starsenrich the interstellar medium with large amounts of processed elements andvarious types of dust. We present the first study on the influence ofgas-to-dust drift on ab initio simulations of stellar winds of M-type starsdriven by radiation pressure on forsterite particles. Our study is based on ourradiation hydrodynamic model code T-800 that includes frequency-dependentradiative transfer, dust extinction based on Mie scattering, grain growth andablation, gas-to-dust drift using one mean grain size, a piston that simulatesstellar pulsations, and an accurate high spatial resolution numerical scheme.To enable this study, we calculated new gas opacities based on the ExoMoldatabase, and we extended the model code to handle the formation of mineralsthat may form in M-type stars. We determine the effects of drift by comparingdrift models to our new and extant non-drift models. Three out of four newdrift models show high drift velocities, 87-310 km/s. Our new drift modelmass-loss rates are 1.7-13 per cent of the corresponding values of ournon-drift models, but compared to the results of two extant non-drift modelsthat use the same stellar parameters, these same values are 0.33-1.5 per cent.Meanwhile, a comparison of other properties such as the expansion velocity andgrain size show similar values. Our results, which are based onsingle-component forsterite particles, show that the inclusion of gas-to-driftis of fundamental importance in stellar wind models driven by such transparentgrains. Assuming that the drift velocity is insignificant, properties such asthe mass-loss rate may be off from more realistic values by a factor of 50 ormore.

Three-component modelling of O-rich AGB star winds I. Effects of drift using forsterite