Supersymmetric Dark Matter


A large number of independent astronomical observations (on galactic halos, clusters of galaxies, large scale structures) indicate that in our Universe the average density of matter, normalized to the critical density ρc = 1.88 · 10 −29 h g · cm (h is the Hubble constant in units of 100 km · s ·Mpc), is in the range 0.2 < ∼ Ωm < ∼ 0.4 (or equivalently, 0.05 < ∼ Ωmh 2 < ∼ 0.3) [1]. The value Ωm ∼ 0.3 may also be derived by combining CMB measurements [2] with data on highredshift SNIa [3], with the further result that a large value, ΩΛ ∼ 0.7, should be assigned to the cosmological-constant (or quintessence) contribution. By comparing these results on Ωm with the contribution to matter provided by visible matter, Ωvis ∼ 0.003, and with the amount of baryonic matter, as deduced from primordial nucleosynthesis, Ωb < ∼ 0.05 [4], one concludes that: i) most of the matter in the Universe is dark, ii) only a small fraction of it is baryonic. Particle physics offers a large selection of possible candidates for dark matter, once one considers extensions of the Standard Model (SM). The most obvious option is represented by massive neutrinos, as suggested by oscillation effects observed in solar and atmospheric neutrinos (for the latest data, see Ref.[5] and Ref.[6], respectively). In these experiments only differ-

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Cite this paper

@inproceedings{Bottino2002SupersymmetricDM, title={Supersymmetric Dark Matter}, author={A Bottino and F Donato and N Fornengo and S Scopel}, year={2002} }