Structure and Circulation of Self-gravitating Toroids

Astronomy and Astrophysics – Astronomy

Scientific paper

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Accretion, Accretion Disks, Hydrodynamics

Scientific paper

We present a numerical scheme to calculate the stationary structure of and the meridional flow in self gravitating pseudo-barotropic toroids. We have applied this scheme to compute simplified models of toroids surrounding a central point mass of 1.4 Msun. The opacity of matter in the toroids is assumed to be only due to electron scattering, and energy generation processes in the toroids are crudely approximated assuming two types of energy sources: (i) a ringlike source which resembles Cowling's model in the case of (spheroidal) stars, and (ii) a viscous heating source which mimics energy generation in accretion disks.
Toroids with the ringlike energy source possess a convective core and a radiative envelope, while those with the viscous heating source do not show a convective core, if the temperature in the core of the toroid is low enough that radiation pressure is negligible. Angular variations of the temperature gradient in the radiative envelope of the toroids excite a meridional flow similar to the well-known meridional circulation found in stars. For toroids with the viscous heating source we find two branches of equilibrium configurations if the specific angular momentum is constant throughout the toroid. One equilibrium branch is characterized by toroids having a small size and a small mass, while in the other branch both the size and the mass of the toroids are large.

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