| Line | After evidence was obtained in the 1920s that |
| the universe is expanding, it became reasonable to | |
| ask: Will the universe continue to expand | |
| indefinitely, or is there enough mass in it for the | |
| (5) | mutual attraction of its constituents to bring this |
| expansion to a halt? It can be calculated that the | |
| critical density of matter needed to brake the | |
| expansion and close the universe is equivalent | |
| to three hydrogen atoms per cubic meter. But the | |
| (10) | density of the observable universe—luminous |
| matter in the form of galaxies—comes to only a | |
| fraction of this. If the expansion of the universe is | |
| to stop, there must be enough invisible matter in | |
| the universe to exceed the luminous matter in | |
| (15) | density by a factor of roughly 70. |
| Our contribution to the search for this missing | |
| matter has been to study the rotational velocity of | |
| galaxies at various distances from their center of | |
| rotation. It has been known for some time that | |
| (20) | outside the bright nucleus of a typical spiral galaxy |
| luminosity falls off rapidly with distance from the | |
| center. If luminosity were a true indicator of mass, | |
| most of the mass would be concentrated toward | |
| the center. Outside the nucleus the rotational | |
| (25) | velocity would decrease geometrically with |
| distance from the center, in conformity with | |
| Keplers law. Instead we have found that the | |
| rotational velocity in spiral galaxies either remains | |
| constant with increasing distance from the center | |
| (30) | or increases slightly. This unexpected result |
| indicates that the falloff in luminous mass with | |
| distance from the center is balanced by an | |
| increase in nonluminous mass. | |
| Our findings suggest that as much as 90 percent | |
| (35) | of the mass of the universe is not radiating at any |
| wavelength with enough intensity to be detected | |
| on the Earth. Such dark matter could be in the | |
| form of extremely dim stars of low mass, of large | |
| planets like Jupiter, or of black holes, either small | |
| (40) | or massive. While it has not yet been determined |
| whether this mass is sufficient to close the universe, | |
| some physicists consider it significant that estimates | |
| are converging on the critical value. |