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1
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84927270874
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For an introductory review, see, e.g., J. R. Primack, in From Nuclei to Stars, proceedings of the Enrico Fermi International School of Physics, Varenna, Italy, 1984, edited by A. Molinari and R. A. Ricci (North-Holland, Amsterdam, 1985), Vol. 91.
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11
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84927270873
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IMB Collaboration report 1986 (unpublished);
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12
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84927270872
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Kamiokande Collaboration report, 1987 (unpublished).
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13
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84927270871
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F. T. Avignone III et al., in Weak and Electromagnetic Interactions in Nuclei, proceedings of the International Symposium, Heidelberg, West Germany, 1986, edited by H. V. Klapdor (Springer, New York, 1987);
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15
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84927270870
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D. O. Caldwell, in Neutrino Masses and Neutrino Astrophysics, proceedings of the Fourth Telemark Conference, Ashland, Wisconsin, 1987, edited by V. Barger et al. (World Scientific, Singapore, 1987), p. 262;
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16
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84927270869
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D. O. Caldwell et al. (in preparation).
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22
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84927270868
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edited by, R. Donaldson, J. Marx, Division of Particles and Fields of the APS, New York
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(1987)
Proceedings of the Summer Study on Physics of the Superconducting Super Collider, Snowmass, Colorado, 1986
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Cabrera, B.1
Caldwell, D.2
Sadoulet, B.3
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26
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84927270865
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We should mention that modulation is not the only means for distinguishing a WIMP signal from background. For example, varying the atomic weight of the target will yield information about the mass and identity of incident particles. In addition, bolometric detectors may have sufficient spatial and energy resolution to help distinguish a signal from radioactive backgrounds. See Refs. 4 and 5.
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32
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84927270864
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These models assume an isothermal halo with a scale height a apeq 4 – 5 kpc. We assume throughout that the halo density is due solely to WIMP's.
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33
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84927270863
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Joel Primack (private communication);
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34
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84927270862
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G. R. Blumenthal, in Nearly Normal Galaxies: from the Planck Time to the Present, proceedings of the Eighth Summer Workshop, Santa Cruz, California, 1986, edited by S. Faber (unpublished). For earlier discussions of halo infall, see B. S. Ryden and J. E. Gunn, in Dark Matter in the Universe, proceedings of IAU Symposium No. 117, Princeton, New Jersey, 1985, edited by J. Kormendy and G. R. Knapp (Reidel, Boston, 1987);
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36
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84927270861
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It appears that halo infall will enhance the distribution in the radial direction;
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37
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84927270860
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according to Ref. 5, this increases the modulation rate. Thus, in terms of detecting modulation, the isotropic Gaussian distribution is very probably a worst-case scenario in comparison to more realistic models.
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39
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84927270859
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Note that we are neglecting the effects of the solar and Earth gravitational fields on the WIMP distribution. Since we are concerned in this paper with WIMP's of initial kinetic energy much higher than their gravitational potential energy, this approximation is justified.
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42
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84927270858
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Fermilab report 1988 (unpublished). The error in the estimate of t=0 comes from the uncertainty in the solar motion with respect to the local standard of rest.
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Griest, K.1
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43
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84927270857
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See Ref. 10. Note that it is only for coherently interacting WIMP's that very massive nuclei are desirable and thus coherence loss must be considered. For particles with only spin-dependent interactions, on the other hand, the most desirable detector nuclei are those that maximize energy loss, i.e., which match nuclear and WIMP masses. In this case, relatively small nuclear masses are desirable.
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46
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84927270856
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We note that in Eqs. (4.3), (4.4), and (4.6) there is a more complicated but slight dependence on the halo and solar velocities which we have not displayed. Also note that in these equations, the approximate relation M = 0.931 (Z+N) GeV between nuclear mass and atomic number has been used. In the figures, the exact nuclear masses are used.
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55
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84927270855
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See, e.g., Srednicki, Olive, and Silk (Ref. 2).
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56
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4243983040
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This calculation was first carried out schematically by Goodman and Witten (Ref. 4). Our discussion here follows that of Srednicki, Olive, and Silk (Ref. 2), and
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(1986)
Nucl. Phys.
, vol.277 B
, pp. 525
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Kane, G.1
Kani, I.2
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57
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84927270854
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We note that in models with significant mixing between left- and right-handed squarks, photinos would have coherent interactions with nuclei.
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58
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84927270853
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UA1 Collaboration, S. P. Geer et al.., talk presented at the International Europhysics Conference on High Energy Physics, Uppsala, Sweden, 1987 (unpublished); UA1 Collaboration, C. J. Seez et al.., talk presented at the second Topical Seminar on Heavy Flavor Physics, San Miniato, Italy, 1987 (unpublished).
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59
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84927270852
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EMC Collaboration, talk presented at Uppsala Conference (Ref. 22); J. Ellis, ibid. We thank Howie Haber for bringing this reference to our attention.
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60
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84927270851
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Sadoulet, Rich, Spiro, and Caldwell (Ref. 4).
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61
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0006280086
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The structure of star clusters. II. Steady-state velocity distributions
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In actuality, the distribution function will not be truncated discontinuously, but will instead go smoothly to zero as the escape velocity is approached. See, for example
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(1965)
The Astronomical Journal
, vol.70
, pp. 376
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King, I.R.1
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62
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84927270850
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However, for our purposes, the distribution (A1) is an excellent approximation to a King model.
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