Theory of Steady Accretion Disks

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Abstract
Theory of steady accretion disks is extended to cover wide ranges of the mass of the central star and of the accretion rate. At first the physical states of the accretion disks based on the standard accretion disk model are summarized for the cases of low through high accretion rates. When the accretion rate is increased beyond a certain critical value which depends on the mass of the central star, inner disk tends to geometrically thick; the standard accretion disk model cannot be applied. In this paper we advance, in addition, a theory which can be applied to geometrically thick accretion disks. One of the distinct properties of the thick disk is super-critical accretion, which presumably produces high speed plasma jets in the directions perpendicular to the disk surface, due to production of super-Eddington flux emerged in the vicinity of the inner boundary of the disk, especially, surrounding a black hole of mass 108M⊙.

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