Motion of gaseous dust grains in triaxial rotating galaxies

Details Motion of gaseous dust grains in triaxial rotating galaxies Motion of gaseous dust grains in triaxial rotating galaxies

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994arep...38..329a&link_type=abstract

Astronomy Reports, Volume 38, Issue 3, May 1994, pp.329-333

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The fall of gaseous dust matter in triaxial rotating galaxies results in the formation of elliptical disks of gaseous dust. Such disks are formed in the central region and lie in the equatorial plane or in the meridional plane and rotate about the principle vertical axes of the galaxy. The computed field of velocities demonstrates rotation and expansion of the disks. The appearance of local counterflows of gaseous dust matter with respect to stars is probable.

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