Gaseous Vortices in Barred Spiral Galaxies

Details Gaseous Vortices in Barred Spiral Galaxies Gaseous Vortices in Barred Spiral Galaxies

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995nyasa.773..320e&link_type=abstract

Waves in Astrophysics, vol. Volume 773, p. 320-328

Astronomy and Astrophysics

Astrophysics

Galactic Structure, Spiral Galaxies, Corotation, Gas Flow, Lagrangian Function, Three Dimensional Models, Velocity Distribution, Vortices, Hydrodynamics, Libration, Mass Distribution

Scientific paper

During the course of examining many two-dimensional, as well as a smaller sample of three-dimensional, models of gas flows in barred spiral galaxies, we have been impressed by the ubiquitous presence fo vortex pairs, oriented roughly perpendicular to their bars, with one vortex on each side. The vortices are obvious only when viewed in the bar frame, and the centers of their velocity fields usually are near Lagrangian points L4,5. In all models that we have studied, the vortices form on essentially the same time scale as that for the development of gaseous spiral arms, typically two bar rotations. Usually the corotation radius, rc, lies slightly beyond the end of the bar. Depending upon the mass distributions of the various components, gas spirals either into, or out of, the vortices: In the former case, the vortices become regions of high density, whereas the opposite is true if the gas spirals out of a vortex. The models described in this paper have low-density vortices, as do most of the models we have studied. Moreover, usually the vortex centers lie approximately within +/- 15 deg of L4,5. In the stellar dynamic limit, when pressure and viscous forces are absent, short-period orbits exist, centered on L4,5. These orbits need not cross and therefore their morphology is that of gas streamlines, that is, vortices. We believe that the gas vortices in our models are hydrodynamic analogues of closed, short-period, libration orbits centered on L4,5.

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