Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...324...60b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 324, Jan. 1, 1988, p. 60-74. Research supported by the University of Virgin
Astronomy and Astrophysics
Astrophysics
46
Disk Galaxies, Dynamic Stability, Galactic Structure, Gas Dynamics, Interstellar Gas, Spiral Galaxies, Density Distribution, Euler Equations Of Motion, Perturbation Theory
Scientific paper
A general local dynamical stability analysis for interstellar gas flow through the spiral arm regions in disk galaxies is presented. A polytropic single-fluid treatment is used. All perturbation wavenumbers in the plane of the disk are considered. It is found that there are preferred directions of growth in spiral arm flow. The directions are roughly along the arm and perpendicular to the arm, with a slight bias toward initially leading configurations. Swing amplification in general has two root causes: shear and divergence flow. Reverse shear (angular velocity increasing outward) is generally present in regions of strong compression and disrupts classical swing amplification. The relative as well as absolute rates of growth in the two predominant directions depend upon the underlying flow stability. Very unstable flow favors growth along the arm. More stable flow seems to prefer growth perpendicular to the arms, leading to branches or spurs.
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