Abstract We consider the effects of advection, radial gradients of pressure and radial drift velocity on the structure of accretion disks around black holes. Models with large accretion rate are investigated, where there is no continuous local solution. Continuous solutions for advective disks exist for all accretion rates. Despite the importance of advection on it's structure, the disk remains geometrically thin.
Keywords accretion disks: advection: radiative transfer
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