A neutrino telescope is well suited to the indirect detection of non baryonic
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
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.