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log (Cross Section/10 cm )
-38 2
10
8
6
4
2
0
σ ν
ΤΟΤ
Ν
log (Neutrino Energy/GeV)
10
ν e
6.4 PeV
e W
4 6 8 10
Figure 3: Cross section at the Glashow resonance and total cross section for neutrino-nucleon interaction.
3.1.5 Neutralino annihilation
Weakly interacting massive particles (WIMPs) could constitute the cold component of the
dark matter in the Universe. Massive supersymmetric neutralinos in the GeV-TeV range are
promising candidates for these particles, and could e.g. be indirectly detected by the observation
of their annihilation products.
Neutralinos accumulated in the galactic halo can lose energy by elastic scattering off nuclei
and get trapped gravitationally in heavy objects, like the Sun or the Earth. Their density then
increases as well as their annihilation rate, until a reservoir is formed. Equilibrium is achieved in
the case of the Sun. Neutralinos can annihilate to normal particles (leptons, quarks, gluons) and
to gauge and Higgs bosons, for the heavier masses. Hadronization or decay of these annihilation
products then produce high-energy neutrinos [25]. These neutrinos can in turn produce muons
by charge current interaction with matter and be detected with a neutrino telescope. Neutralinos
could thus be detected by observing an excess of events coming from the center of the Sun or
the Earth above a background of atmospheric neutrinos. The non-observation of such an excess
would then make it possible to rule out some theoretical models predicting it [25].
10