Hooper, Dan and Petriello, Frank and Zurek, Kathryn M. and Kamionkowski, Marc (2009) New DAMA dark-matter window and energetic-neutrino searches. Physical Review D, 79 (1). Art. No. 015010. ISSN 0556-2821. http://resolver.caltech.edu/CaltechAUTHORS:20090413-094317493
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Recently, the DAMA/LIBRA Collaboration has repeated and reinforced their claim to have detected an annual modulation in their signal rate, and have interpreted this observation as evidence for dark-matter particles at the 8.2σ confidence level. Furthermore, it has also been noted that the effects of channeling may enable a weakly interacting massive particle (WIMP) that scatters elastically via spin-independent interactions from nuclei to produce the signal observed by DAMA/LIBRA without exceeding the limits placed by CDMS, XENON, CRESST, CoGeNT, and other direct-detection experiments. To accommodate this elastic-scattering explanation, however, the mass of the responsible dark-matter particle must be relatively light, mDM ≾ 10 GeV. Such dark-matter particles will become captured by and annihilate in the Sun at very high rates, leading to a potentially large flux of GeV-scale neutrinos. We calculate the neutrino spectrum resulting from WIMP annihilations in the Sun and show that existing limits from Super-Kamiokande can be used to close a significant portion of the DAMA region, especially if the dark-matter particles produce tau leptons or neutrinos in a sizable fraction of their annihilations. We also determine the spin-dependent WIMP-nuclei elastic-scattering parameter space consistent with DAMA. The constraints from Super-Kamiokande on the spin-dependent scenario are even more severe—they exclude any self-annihilating WIMP in the DAMA region that annihilates 1% of the time or more to any combination of neutrinos, tau leptons, or charm or bottom quarks.
|Additional Information:||© 2009 The American Physical Society. Received 5 September 2008; published 22 January 2009. D. H. is supported by the Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy and by NASA Grant No. NNX08AH34G. M. K. is supported by DOE Grant No. DE-FG03-92-ER40701 and the Gordon and Betty Moore Foundation. F. P. and K. M. Z. are supported by DOE Grant No. DE-FG02-95ER40896. F. P. and K. M. Z. thank the Aspen Center for Physics, where part of this work was completed.|
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|Deposited By:||Tony Diaz|
|Deposited On:||20 Apr 2009 22:35|
|Last Modified:||26 Dec 2012 10:57|
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