Self-consistent mass-loss solutions are computed for post-AGB stars, and the evolution of the central star is followed by utilizing the sequences of the steady mass-loss and the static solutions. The mass loss is driven by the radiation pressure gradient and the matter is accelerated in the inner region to the photosphere. The optically thick wind occurs when the H-burning luminosity is larger than the Eddington limit at the surface region. Such a situation is realized in the low-temperature region of the H-R diagram. Therefore no wind solution exists when the surface temperature becomes high enough.