Dark Matter

Our galaxy, the Milky Way, and other galaxies contain more matter than expected from visual observations.  This so called "dark matter" is detected by the rapid rotation of matter in the outer regions of galaxies as well as the motion of the galaxies within galactic clusters.  The gravity exerted by the dark matter holds the galaxies and clusters together and allows faster rotations than would be possible if it did not exist.  It is estimated that 70% to 90% of the mass which should exist according to the laws of gravity cannot be seen in visible light images of the galaxies.
 

Candidates for the dark matter include:

But when all the estimates of the masses of these different classes of objects is joined together it still does not provide enough mass to explain the gravitational effects observed in galaxies and clusters of galaxies.  Physicists have invented several possible catagories for the remaining missing dark matter: A variety of observational methods may be used to detect and differentiate between the various dark matter candidates.  These include:

Missing Mass Pages

Dark Matter Pages

MACHO Pages

WIMP Pages

superWIMP Pages

Gravitational Microlensing Pages

Brown Dwarf Pages

Red Dwarf Pages

White Dwarf Pages

Neutron Star Pages

Black Hole Pages

Neutrino Experiments

Interstellar Gas Clouds

Gravity Wave Detectors


Related Pages

Stellar Evolution

Observatories and Sky Surveys

Globular Cluster Distance & Ages



Astronomy Index

Created: February, 1998
Last Modified: July 9, 2003
HTML Editor: Robert Bradbury