Hydrodynamical winds from an accretion disk

Physics – Plasma Physics

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Accretion Disks, Computerized Simulation, Hydrodynamics, Stellar Winds, Boundary Value Problems, Finite Difference Theory, Magnetohydrodynamic Flow, Plasma Density, Radiation Pressure

Scientific paper

Numerical simulations of thermally driven winds originating in a disk round a compact object are performed. The disk is assumed to be geometrically thin, self similar under scaling in radius, and in a dynamical balance. A polytropic relation between density and pressure is assumed. Steady state solutions are obtained for appropriate boundary conditions. It is found that a cone where the density and the pressure become extremely low is formed around the rotation axis, if the disk has angular momentum. While a large portion of the flow is outgoing, gas originating in the inner disk falls into the central gravitating object. In order for the disk winds to blow, the pressure and density distributions at the disk are restricted in some range.

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