Neutrinos from dark matter

A neutrino telescope is well suited to the indirect detection of non baryonic dark matter. In the MSSM the supersymmetric partners of the neutral bosons are four neutralinos: the two partners of the neutral SU(2) gauge bosons (gauginos), and the two partners of the neutral Higgs particles (higgsinos). The lightest neutralino is a linear combination of these four states. The neutralinos remnants from the Big Bang move in the halo of the Galaxy with velocity of few hundreds of km/s and loose energy by elastic scattering on the nuclei forming the matter of the Sun and of the Earth when they cross them. This will result in a high concentration of neutralinos in these celestial bodies enhancing the annihilation rate per volume unit which will produce the neutrino emission. The signal will, thus, consist in an excess of neutrino flux coming from the Sun or from the center of the Earth. The calculation of the sensitivity of a detector must take into account all the parameters of the theoretical model and of the physical background of atmospheric neutrinos. This calculation has been performed in ref.~[#bottino##1#] in terms of the sensitive area required to detect a four standard deviations signal as a function of the neutralino mass. The results of this calculation show (see figures 12 and 14 of ref.~[#bottino##1#]) that a detector with an area of 1km#tex2html_wrap_inline726# running for one year would be sensitive to a range of neutralino masses extending up to few TeV.