Abstract:
In an earlier paper (Prabhu and Krishan 1994) a model of the flat rotation curves of galaxies has been given. This model attempts to explain the rotation curves without invoking dark matter, instead it depends on certain properties of a turbulent medium. It is felt that some issues related to Keplerian motion have remained unaddressed. In this paper, by going into the local Keplerian frame, the equations for turbulent motions are derived. In our earlier work we used these equations to obtain the turbulent energy spectrum. Thus, the contributions of Keplerian and turbulent motions are required to account for the flat rotation curves of galaxies.
