The nature of accretion is of fundamental interest in the study of supermassive black holes in AGN and stellar mass black holes in black hole X-ray binary systems.The accretion process in these two classes of objects is thought to be similar,however,there are several observational differences that are difficult to interpret within the same framework.We explore the possibility that the accretion flow is described by more than one gaseous component,given that the physical state of gas in the central regions of galaxies is characterized by both hot,ionized and cool molecular gas components.As a first examination of this model,we consider the limiting case of the flow as a geometrically thick coronal gas component supplied by gravitational capture of interstellar medium or stellar wind,and study its condensation to a geometrically thin cold disk before accretion onto the supermassive black hole.We found that for mass accretion rates less than about 0.01(expressed in Eddington units),condensation does not occur and the accretion flow takes the form of a corona/ADAF.For higher mass accretion rates(> 0.02),the coronal mass flow rate decreases and the cool mass flow rate increases with decreasing radius.Here the hot gas partially condenses to the cooler regions characterizing the underlying disk as it flows towards the black hole.For accretion rates of order 0.1,the mass flow rate of the coronal gas attains values of order 0.02 in the innermost regions of the disk,which can help to elucidate the production of strong X-ray with respect to the optical and ultraviolet radiation in high luminosity AGN,without assuming a large fraction of disk accretion energy is transferred to the corona.