Time-dependent accretion disks around compact objects. I - Theory and basic equations. II - Numerical models and instability of inner region

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Abstract

We consider accretion disks around compact stars and black holes, generalizing the stationary disk models of various authors to allow time dependence on the radial-flow time scale. The structure and evolution of the disk are governed by an 'evolution equation' for matter surface density, plus a set of implicit algebraic equations determining various thermodynamic and radiation variables in terms of surface density. The analytic structure of these equations is studied. It is shown that there exists a maximum permissible value of the surface density at which gas and radiation pressure are approximately equal, and beyond which viscosity generates more energy than radiative transport can remove.

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