Authors: Geoffrey M. Williams
A spiral galaxy is modeled as a thin, flat, axisymmetric disk comprising a series of concentric, coplanar rings. Using conventional Newtonian gravitation kinematics, it is shown that relatively flat velocity curves are produced by a variety of possible mass distributions in the disk. No halo of "dark matter" is needed to produce these rotation curves. Compared with a point mass at the center, the disk gravitational force grows with increasing distance from the disk center, crests and then slowly subsides beyond the disk perimeter. The model is applied to the NGC 3198, M31 and NGC 4736 galaxies, with ring masses adjusted to match the respective velocity profiles. Gravitational force fields in the disk are calculated, leading to direct estimates of enclosed galaxy mass. The mass distributions of several other spiral galaxies are analyzed, and their basic characteristics are charted in Appendix 2.
Comments: 29 pages.
Unique-IP document downloads: 1081 times
Vixra.org is a pre-print repository rather than a journal. Articles hosted may not yet have been verified by peer-review and should be treated as preliminary. In particular, anything that appears to include financial or legal advice or proposed medical treatments should be treated with due caution. Vixra.org will not be responsible for any consequences of actions that result from any form of use of any documents on this website.
Add your own feedback and questions here:
You are equally welcome to be positive or negative about any paper but please be polite. If you are being critical you must mention at least one specific error, otherwise your comment will be deleted as unhelpful.