Computer Science – Sound
Scientific paper
Dec 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apjs...41..635w&link_type=abstract
Astrophysical Journal Supplement Series, vol. 41, Dec. 1979, p. 635-667.
Computer Science
Sound
3
Density Wave Model, Disk Galaxies, Flow Stability, Galactic Rotation, Galactic Structure, Hydrodynamics, Interstellar Gas, Coriolis Effect, Differential Equations, Eigenvalues, Halos, Pitch (Inclination)
Scientific paper
This paper deals with the stability of the boundary layer circulation of interstellar gas in a galaxy. This flow was derived in a previous work concerning a rotating axisynimetric galaxy containing a gaseous disk embedded in a surrounding gaseous halo. There it was shown that a boundary layer circulation exist in the meridional plane, this flow extending from the galactic plane to several disk scale heights into the halo. Shear-flow instabilities are expected because of the presence of inflection points in the vertical structure of this flow. In this paper we derive the differential eigenvalue equations governing linear waves of arbitrary pitch angle in a (spatially) slowly varying medium. The wave dynamics are constrained by the Boussinesq approximation insofar as the adopted scaling filters out sound waves and suppresses the effects of self-gravity while preserving the buoyancy effects. By suitably defining certain quantities locally, we are able to cast the characteristic-value problem in a form which is similar to other well-known problems in the theory of shear-flow instability. Solutions of the governing equations are considered in a separate paper.
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