$U(1)_{B-L}$ Sneutrino Dark Matter Detection with the IceCube Neutrino Telescope

Details $U(1)_{B-L}$ Sneutrino Dark Matter Detection with the IceCube Neutrino Telescope $U(1)_{B-L}$ Sneutrino Dark Matter Detection with the IceCube Neutrino Telescope

2009-12-07

arxiv.org/abs/0912.1324v1

Physics

High Energy Physics

High Energy Physics - Phenomenology

Presented at CCAPP Symposium 2009, Columbus, OH - 6 pages, 2 figures

Scientific paper

We investigate the prospects for indirect detection of right-handed sneutrino dark matter at the IceCube neutrino telescope in a $U(1)_{B-L}$ extension of the MSSM. The capture and annihilation of sneutrinos inside the Sun reach equilibrium, and the flux of produced neutrinos is governed by the sneutrino-proton elastic scattering cross section, which has an upper bound of $8 \times 10^{-9}$ pb from the $Z^{\prime}$ mass limits in the $B-L$ model. Despite the absence of any spin-dependent contribution, the muon event rates predicted by this model can be detected at IceCube since sneutrinos mainly annihilate into leptonic final states by virtue of the fermion $B-L$ charges. These subsequently decay to neutrinos with 100% efficiency. The Earth muon event rates are too small to be detected for the standard halo model irrespective of an enhanced sneutrino annihilation cross section that can explain the recent PAMELA data. For modified velocity distributions, the Earth muon events increase substantially and can be greater than the IceCube detection threshold of 12 events $\mathrm{km}^{-2}$ $\mathrm{yr}^{-1}$. However, this only leads to a mild increase of about 30% for the Sun muon events. The number of muon events from the Sun can be as large as roughly 100 events $\mathrm{km}^{-2}$ $\mathrm{yr}^{-1}$ for this model.

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