Explaining PAMELA and WMAP data through coannihilations in extended SUGRA with collider implications
- Department of Physics, Northeastern University, Boston, Massachusetts 02115 (United States)
- C. N. Yang Institute for Theoretical Physics, Stony Brook University, Stony Brook, New York 11794 (United States)
The PAMELA positron excess is analyzed within the framework of nonuniversal supergravity (SUGRA) models with an extended U(1){sup n} gauge symmetry in the hidden sector leading to neutralino dark matter with either a mixed Higgsino-wino lightest R-parity odd supersymmetric particle (LSP) or an essentially pure wino-dominated LSP. The Higgsino-wino LSP can produce the observed PAMELA positron excess and satisfy relic density constraints in the extended class of models due to a near degeneracy of the mass spectrum of the extended neutralino sector with the LSP mass. The simultaneous satisfaction of the WMAP relic density data and the PAMELA data is accomplished through a coannihilation mechanism (B{sub Co}-mechanism), and leads to predictions of a neutralino and a chargino in the mass range (180-200) GeV as well as low-lying sparticles accessible at colliders. We show that the models are consistent with the antiproton constraints from PAMELA as well as the photon flux data from EGRET and FERMI-LAT. Predictions for the scalar neutralino-proton cross section relevant for the direct detection of dark matter are also discussed and signatures at the LHC for these PAMELA inspired models are analyzed. It is shown that the mixed Higgsino-wino LSP model will be discoverable with as little as 1 fb{sup -1} of data and is thus a prime candidate for discovery in the low luminosity runs at the LHC.
- OSTI ID:
- 21325261
- Journal Information:
- Physical Review. D, Particles Fields, Vol. 80, Issue 7; Other Information: DOI: 10.1103/PhysRevD.80.075001; (c) 2009 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA); ISSN 0556-2821
- Country of Publication:
- United States
- Language:
- English
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