Abstract
Rotation curves contain information about the early dynamical history of galaxies. We calculate quasi-stationary rotation curves for highly turbulent, gaseous, non-magnetic proto-galaxies which are acted upon by external torques. These torques arise from nearby condensations. The detailed structure of the curves can vary widely; it depends mainly upon the relative strengths of torque and turbulence and upon the initial density distribution. However, nearly all the rotation curves share a similar general form. The central regions of the proto-galaxy have constant angular velocity, intermediate regions have varying angular velocity, and outer regions tend to a different constant angular velocity. The main observed properties of rotation curves for evolved Sb and Sc galaxies can be reproduced if the initial density and viscosity distributions are not strongly centrally concentrated, if initial turbulent velocities are less than several hundred km s –1 , if the central solid-body regions of proto-galaxies do not contract substantially as they evolve with detailed angular momentum conservation, and if the outer regions evolve non-homologously.
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