Meridional flow in a self-gravitating body. I - Mechanical flow in a barotropic star with constant specific angular momentum

Details Meridional flow in a self-gravitating body. I - Mechanical flow in a barotropic star with constant specific angular momentum Meridional flow in a self-gravitating body. I - Mechanical flow in a barotropic star with constant specific angular momentum

Nov 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...168..130e&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 168, no. 1-2, Nov. 1986, p. 130-138.

Astronomy and Astrophysics

Astrophysics

11

Angular Momentum, Barotropic Flow, Meridional Flow, Stellar Gravitation, Stellar Models, Stellar Rotation, Accretion Disks, Incompressible Fluids, Pressure Effects, Stellar Structure, Stream Functions (Fluids), Vorticity Equations

Scientific paper

The mechanical part of the equations governing meridional circulation in a self-graviting body is solved. Stationary axisymmetric solutions are computed neglecting the effects of viscosity and assuming that the fluid is incompressible and has a constant specific angular momentum. Then, the vorticity has a simple relation to the stream function. Three types of models are investigated: (1) nonrotating configurations of spherical topology which are deformed due to the internal motion (pure circulation case); (2) rotating configurations of toroidal topology; and (3) models consisting of a rotating toroidal configuration and a central point mass (accretion disk case). Assuming appropriate choices of the vorticity stream function relation, several stationary sequences are computed. The models obtained contain one or several large scale circulations in the meridional plane. The configuration change due to circulation is small, i.e., the shape is mainly determined by three forces, the pressure gradient, the gravity, and the centrifugal force.

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