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A Newtonian version of the theory of thick accretion disks orbiting black holes is described. In view of the present inadequate knowledge of microscopic viscosity processes, this theory adopts a macroscopic approach. All the uncertainties are absorbed in currently arbitrary functions lambda (xi) and f(xi) which describe the (non-Keplerian) angular momentum along the disk, and the outgoing radiation flux in units of the critical flux. Assuming surface distributions of angular momentum and radiation flux, a model of a thick, non-Keplerian accretion disk can be constructed with no knowledge of the viscosity mechanism. Thick accretion disks can have luminosities 100 times above the Eddington limit. Self-consistency constraints for the theory of thick accretion disks with super-Eddington luminosities are studied.
Abramowicz et al. (Mon,) studied this question.