Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...265..402h&link_type=abstract
Astrophysical Journal, Part 1, vol 265, Feb. 1, 1983, p. 402-416.
Astronomy and Astrophysics
Astrophysics
10
Rotating Fluids, Stellar Envelopes, Stellar Models, Viscous Flow, Vorticity, Computerized Simulation, Disks (Shapes), Inviscid Flow, Linear Equations, Shear Properties
Scientific paper
An approximate algebraic method is presented for determining when local, self-gravitating structures can develop in viscous, shearing media, such as disks that may be generated by computer simulation. The principal advantage of the technique is that it does not require the numerical solution of the linear differential equations. This is seen as being of signal importance in the present context, since the general local problem considered here is characterized by five independent parameters. It is shown that the vorticity modes can grow spectacularly in viscous disks. Indeed, with significant shear viscosity, the familiar density waves damp strongly and only vortices survive. Therefore, the growth of structure in circumstellar disks and in the solar nebula may have proceeded along fundamentally different lines from those of the density enhancements in the disks of galaxies.
Horak T.
Hunter James H. Jr.
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