Free Resources |
||||||||||||||||
|
||||||||||||||||
The following HTML text is provided to enhance online readability. Many aspects of typography translate only awkwardly to HTML. Please use the page image as the authoritative form to ensure accuracy. the expected power deposited by a “KSVZ” axion should the axion have the corresponding mass. Notice the experiment sensitivity is approaching 10-23 W, well below the line. ConclusionsOver the last year, WIMP and axion searches became sensitive enough to detect plausible dark matter candidates. The WIMP part of this overview focused on the CDMS effort. The axion part of this overview focused on the California effort. There are numerous other experiments, but brevity did not allow me to discuss them in any detail. This is an exciting time for the dark matter community: should copious amounts of dark matter exist as WIMPs or axions, they could be discovered soon. I wish to thank Tom Shutt of the Center for Particle Astrophysics, Berkeley, for helpful discussions and for material relating to the CDMS effort. 1. Kolb, E. & Turner. M. (1990) The Early Universe (AddisonWesley, Reading, PA). 2. Gates. E., Gyuk, G. & Turner, M. (1995) Astrophys. J. 449, 123. 3. Jungman, G. & Kamionkowski, M. (1996) Phys. Rep. 267, 195–373. 4. Turner, M. (1990) Phys. Rep. 197, 67–97. 5. Sikivie, P. (1983) Phys. Rev. D 32, 2988–2991. 6. Wuensch, W.U., DePanfilis-Wuensch, S., Semertzidis, Y.K., Rogers, J.T., Melissinos, A.C., Halama, H.J., Moskowitz, B.E., Prodell, A.G., Fowler. W.B. & Nezrick, F.A. (1989) Phys. Rev. D 40, 3153–3167. 7. Hagmann, C., Sikivie, P., Sullivan, D.B. & Tanner, D.B. (1990) Phys. Rev. D 42, 1297–1300.
|
|
|||||||||||||||
