2001/12/11 by R. Arnowitt, B. Dutta, Arnowitt, R. +1
Physics and Astronomy · #FOS: Physical sciences #High Energy Physics - Phenomenology (hep-ph) #hep-ph
paper · pdf · doi:10.48550/arxiv.hep-ph/0112157
14 pages, latex, 8 figures, talk at COSMO-01, Rovaniemi, Finland, August 29 - September 4, 2001
arxiv created 2001/12/11 · arxiv updated 2009/11/30
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 tanβ< 50, and thus the largest theoretical neutralino-proton cross sections still lie significantly below the DAMA 3σlower bound. (Predictions for tanβ> 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 tanβ< 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 tanβ>~ 15 with mχ01 > 80 GeV, and minimum cross sections >~10-10 pb for μ> 0.