Dark Matter Detection Rates In SUGRA Models

الأصل · EN

Direct detection of Milky Way wimps are discussed within the framework of R-parity conserving SUGRA models with grand unification at MG. Two questions are discussed: what SUGRA models can account for the DAMA data if this data is confirmed, and is the full SUGRA parameter space accessible to future planned detectors. Experimental constraints of the Higgs mass bound, the b-> sγbound, relic density constraints (including all co-annihilation channels), etc. are imposed. In addition, the effect of the possible muon g - 2 anomaly are examined. For mSUGRA, we find that the Higgs mass and b→ sγconstraint puts a lower bound m₁/₂ > (300 - 400) GeV (i.e. mχ⁰₁ > (120 - 160) GeV) for β< 50, and thus the largest theoretical neutralino-proton cross sections still lie significantly below the DAMA 3σlower bound. (Predictions for β> 50 become sensitive to the precise value of mₜ and mb.) If in addition one imposes the muon anomaly constraint, μmust be positive and an upper bound of m₁/₂< 850 GeV for β< 50 is obtained. More generally, if μ>0 and m₁/₂ < 1 TeV, the cross sections are > 10⁻¹⁰ pb, and hence this parameter space would be mostly accessible to planned high sensitivity detectors. For non-minimal SUGRA models, the cross sections can be considerably larger, and a simple SU(5) model with non-universal soft breaking in the Higgs and third generation is seen to give cross sections in the DAMA range for β> 15 with mχ⁰₁ > 80 GeV, and minimum cross sections > 10⁻¹⁰ pb for μ> 0.