  Aspects of the wind-dynamics in symbiotic binaries, colliding winds and
accretion, are reviewed. Inconsistencies between theory and observations of the
hot star wind are discussed. If the hot star wind were governed by CAK theory,
nearly all symbiotics would be colliding wind binaries. For the case of
colliding winds, 3D hydrodynamical simulations reveal that the matter
distribution is spirally shaped. Shock confined high-density shells as well as
huge voids are found even in the immediate neighborhood of the stars. Synthetic
spectra computed on the basis of different 3D hydrodynamical models suggest
observational discrimination between them to be possible. Colliding wind models
also provide a link between symbiotics and planetary nebulae. Accretion during
some time is a necessary condition for symbiotics to exist. However, there is
no proof of whether currently accreting systems show the symbiotic phenomenon.
Existing accretion models are inconsistent amongst each other, predicting
either extended disks or small, high-density accretion wakes. Synthetic spectra
allowing to discriminate between two models do not yet exist.
