Evolution of a central density depression in the stellar disks of galaxies

Details Evolution of a central density depression in the stellar disks of galaxies Evolution of a central density depression in the stellar disks of galaxies

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990azh....67..222z&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 67, Mar.-Apr. 1990, p. 222-229. In Russian.

Astronomy and Astrophysics

Astronomy

1

Density Distribution, Galactic Evolution, Space Density, Stellar Luminosity, Astronomical Models, Brightness Distribution

Scientific paper

A numerical simulation of a three-dimensional collisionless disk by a large number of particles in the field of a static spherical component (the halo) is presented. It is shown that the density depression disappears after two-to-three rotations of the disk if, in the depression region, the ratio of the spherical to the disk component masses is less than about 0.75. The formation of a central density depression in the disks of some galaxies not having a massive bulge appears to be associated with the presence of a bar-mode structure.

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