The softer a potential is, the closer the corresponding Keplerian rotation is to a rigid rotation law. Because of the small radial coupling in such a situation the radial mass flow due to viscosity in an α-accretion disk is very inefficient. Here a model is presented in which the mass of an accretion disk in a soft potential well changes this potential in a sense that an efficient mass flow in radial direction becomes possible, thus making the formation of a centra! mass condensation possib!e. This mechanism is of interest in the context of galactic central regions since it is capable of explaining the existence of centra! masses such as observed in the cores of norma! galaxies; it might aiso be of relevance for the explanation of the activity in AGNs.