Central holes in disks of spiral galaxies

Details Central holes in disks of spiral galaxies Central holes in disks of spiral galaxies

Jan 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980ap%26ss..67...31e&link_type=abstract

Astrophysics and Space Science, vol. 67, no. 1, Jan. 1980, p. 31-43.

Astronomy and Astrophysics

Astronomy

14

Disk Galaxies, Galactic Nuclei, Galactic Rotation, Galactic Structure, Spiral Galaxies, Andromeda Galaxy, Black Holes (Astronomy), Hydrogen Atoms, Interstellar Gas, Mass Distribution, Milky Way Galaxy, Spatial Distribution, Stellar Models

Scientific paper

Rotation curves of the Galaxy, M 31, and M 81 have a deep minimum at a radius of 1-4 kpc. It is demonstrated that this minimum can be dynamically explained if the stellar disks of these galaxies have no representatives in the central region. Such a ring-like distribution of matter in stellar disks is suggested by the similarity observed in the distribution of extreme Population I objects if it is assumed that a stellar disk was formed from a gaseous disk which always had a ringlike structure. The presence of central holes in the disks of spiral galaxies suggests that during the initial collapse phase almost all protogalactic gas with a low angular momentum was consumed to form the spheroidal component. No low-momentum gas was left over to form the stars of the central regions of the disks.

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