Swing amplification of nonaxisymmetric perturbations in stars and gas in a sheared galactic disk

Details Swing amplification of nonaxisymmetric perturbations in stars and gas in a sheared galactic disk Swing amplification of nonaxisymmetric perturbations in stars and gas in a sheared galactic disk

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...390..378j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 390, no. 2, May 10, 1992, p. 378-386.

Astronomy and Astrophysics

Astrophysics

30

Galactic Structure, Interstellar Gas, Perturbation Theory, Shear Flow, Spiral Galaxies, Flow Distortion, Flow Stability, Galactic Rotation, Gas Flow, Hydrodynamics

Scientific paper

A study of the growth of local, nonaxisymmetric perturbations in gravitationally coupled stars and gas in a differentially rotating galactic disk is presented. The physical effects of the inclusion of a low-velocity dispersion component (gas) on the growth of nonaxisymmetric perturbations in both stars and gas are examined. The local, linearized perturbation equations in the sheared frame are solved to obtain the results for a temporary growth via swing amplification. The amplifications and the pitch angles for features in stars and gas are obtained for dynamically distinct cases, as applicable for different regions of spiral galaxies. When the gas contribution is high, the stellar amplification and the range of pitch angles over which it can occur are both increased, due to the gravitational coupling between the two fluids. Thus, the two-fluid scheme can explain the origin of the broad spiral arms in the underlying old stellar populations of galaxies. The arms are predicted to be broader in gas-rich galaxies, as is indeed seen, for example, in M33.

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