Modeling of steady, rotational, transonic winds from rotating stars and galaxies

Details Modeling of steady, rotational, transonic winds from rotating stars and galaxies Modeling of steady, rotational, transonic winds from rotating stars and galaxies

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...267...62k&link_type=abstract

Astrophysical Journal, Part 1, vol. 267, Apr. 1, 1983, p. 62-79.

Statistics

Computation

8

Astronomical Models, Galactic Rotation, Steady Flow, Stellar Rotation, Stellar Winds, Transonic Flow, Computational Fluid Dynamics, Coriolis Effect, Differential Equations, Stellar Models, Stream Functions (Fluids), Vorticity

Scientific paper

The theory of steady transonic winds from condensed bodies is extended to general, two-dimensional, axisymmetric systems. A stream function is used to reduce the gasdynamics equations to a single, second-order differential equation plus an algebraic equation for the density. The approach extends Parker's (1958) quasi-one-dimensional theory, which uses Bernoulli's theorem, to a complete two-dimensional calculation which includes vorticity and rotation. The conceptual basis of the stream function approach is described in detail, and a numerical method for solving the resulting equations is presented. The applications illustrate solutions for stellar (spherical source surface) and galactic (oblate spheroidal source surface) models. Among other things, it is found that for rapidly rotating stellar models the Coriolis force dominates the centrifugal terms and the streamlines bend toward the rotation axis as a consequence of the axisymmetry. For both the rotating and nonrotating galaxy models, the streamlines bend toward the equator.

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