A fluid dynamical flow model for the central peak in the rotation curve of disk galaxies

Details A fluid dynamical flow model for the central peak in the rotation curve of disk galaxies A fluid dynamical flow model for the central peak in the rotation curve of disk galaxies

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980ap%26ss..73..395b&link_type=abstract

Astrophysics and Space Science, vol. 73, no. 2, Dec. 1980, p. 395-410.

Astronomy and Astrophysics

Astrophysics

1

Disk Galaxies, Galactic Nuclei, Galactic Rotation, Gas Dynamics, Angular Velocity, Astronomical Models, Gas Explosions, Hydrodynamic Equations, Interstellar Gas

Scientific paper

The primary peak in the rotation curve of the central region in some dark galaxies is considered as a result of the post-explosion flow pattern of gas in this region. A flow model was constructed using hydrodynamical equations of motion; the model represents the observed linear rotational velocity, followed by the falling branch of the curve to a minimum. The distance of the primary peak from the galactic center correlated with the angular velocity in the linear part of the curve. It was concluded that the distance of the primary peak from the center represents the potential capability of the galaxy nucleus for repeating explosions by a process of mass replenishment at the core.

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