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

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

Dec 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974apj...194..419l&link_type=abstract

Astrophysical Journal, vol. 194, Dec. 1, 1974, pt. 1, p. 419-427, 429-437.

Astronomy and Astrophysics

Astronomy

149

Binary Stars, Black Holes (Astronomy), Magnetohydrodynamics, Rotating Disks, Stellar Gravitation, Time Dependence, Astronomical Models, Density Distribution, Deposition, Neutron Stars, Nonlinear Equations, Plasma Dynamics, Radiative Transfer, Stellar Evolution, Viscosity, X Ray Sources

Scientific paper

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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