Accretion in disk galaxies - The hydrodynamical evolution of molecular rings

Details Accretion in disk galaxies - The hydrodynamical evolution of molecular rings Accretion in disk galaxies - The hydrodynamical evolution of molecular rings

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...235...55d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 235, no. 1-2, Aug. 1990, p. 55-59.

Statistics

Computation

11

Accretion Disks, Computational Astrophysics, Disk Galaxies, Galactic Evolution, Astronomical Models, Galactic Bulge, Galactic Rotation, Magnetohydrodynamics

Scientific paper

A simple hydrodynamical model is presented to explain the formation of molecular rings in galaxies. It uses only the properties of the rotation curves of galaxies, mainly the rigid rotation in the central bulge region. Using the alpha-disk model, this leads to reduced friction and therefore to a lack of angular momentum transport. Since the angular momentum transport is essential for accretion, the accreting masses are slowed down near the transition radius of the rotation curve, therefore forming a ring. It is thus shown why rings coincide with the turnovers in the rotation curves and how rings could be predicted on the basis of the rotation curve.

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