Valluri, Monica (1994) A model for the declining rotation curves of cluster spiral galaxies. In: Astrophysical Journal, 430 (1). pp. 101-106.Full text not available from this repository. (Request a copy)
Recent numerical studies have shown that mean tidal fields in clusters of galaxies can cause a significant increase in the planar velocity dispersions of stars and gas clouds in the disks of spiral galacies. Since the perturbations caused by cluster tidal fields are generally weak and fairly symmetric, the stellar distributions of the perturbed galaxies would not necessarily show obvious signs of tidal disturbance. In this paper it is shown that te increased noncircular velocities of stars can result in a symmetric decline (at large radii) of the rotation curves of tidally perturbed spiral galaxies in clusters. This decline results from the well-known phenomenon of the 'asymmetric drift' of a high velocity dispersion stellar population. This suggests that the observations of the decline rotation curves of spiral galaxies in clusters do not necessarily imply that their dark matter halos have been tidally truncated as in generally assumed.
|Item Type:||Journal Article|
|Additional Information:||The copyright of this article belongs to The American Astronomical Society.|
|Department/Centre:||Division of Information Sciences > Supercomputer Education & Research Centre|
|Date Deposited:||24 Jul 2006|
|Last Modified:||27 Aug 2008 12:15|
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