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The WIMP of a minimal walking Technicolor Theory. J. Virkajärvi Jyväskylä University, Finland. with K.Kainulainen and K.Tuominen. Outline. Technicolor and the WIMP Dynamical Dark Energy and the WIMP density Model results Conclusion & outlook. Basic idea of Technicolor (TC).
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The WIMP of a minimal walking Technicolor Theory J. Virkajärvi Jyväskylä University, Finland with K.Kainulainen and K.Tuominen Spåtind 4.1.2008
Outline • Technicolor and the WIMP • Dynamical Dark Energy and the WIMP density • Model results • Conclusion & outlook
Basic idea of Technicolor (TC) • New gauge interaction TC which only technifermions feel • Left and right handed fermions (massless) have SU(2) • chiral symmetry Technifermion condensate = a composite Higgs (+ (pseudo) Goldstone bosons) Early Universe High Temperature T > TeV Universe expands, T drops • Spontaneus symmetry breaking dynamically • Electroweak symmetry breaking • Right mass ratio for EW gauge bosons
Heavy Neutrino = the WIMP Minimal Walking TC (WTC) • Model: Two techniquarks(flavors) in two index symmetric (= adjoint) presentation of an SU(2) TC gauge group. • Witten anomaly cured by introducing a new Heavy lepton family • Compatible with EW precision measurements (Pure Majorana case) (Sannino & Tuominen, hep-ph/0405209; Dietrich, Sannino & Tuominen, hep-ph/0505059 ) • Near conformal (=walking) FCNC’s suppressed.
Diagonalize two Majorana particles: and (mass eigenstates) for whichand Heavy neutrino mass term • Dirac mass term for charged lepton • For neutrino four cases: 1. Pure Dirac mass term ( ) 2. Pure Majorana mass term (M) 3. Mixed Dirac-Majorana mass term: Two Weyl spinors: 4. Flavor mixed Majorana mass term: Two Weyl spinors: decays to = the WIMP Thermally averaged annihilation cross section:
Dynamical Dark Energy • Dark Energy • Dark Matter • Baryonic Matter • Quintessence: • Dark energy dominates the energy density at early times SM only radiation
SUSY and Our Mixed mass cases Exponential drop Freeze out Our Model SM ”0” means T = 1 MeV Relic density anddynamicaldark energy • Relic density from Lee Weinberg equation • Biggest effects to final abundance of the heavy neutrinos comes from the cross section and Hubble parameter Number density ”0” means T = 1MeV
Model results Pure Dirac Pure Majorana Both cases compatible with nucleosynthesis since r small (for masses shown).
Dotted: Dashed: Solid: Standard expansion Model results (1.approx.) Flavor Mixed Majorana case: Similar results by Kouvaris: (hep-ph/0703266) for neutral bound state between techniquark and technigluon Yellow area Excluded by LEP:
Bound depends on the ratio between local and cosmic WIMP densities Constraints to results • Direct search limits Pure Majorana, (mixed cases) Upper limits for Pure Dirac • Limit from rotation curves + halo models: • lower bound for local density (Jungman, Kamionkowski, Griest, Phys. Rept. 267)
Conclusion and outlook • If a Quintessence-like Dark Energy dominates the early universe evolution • 4th generation dirac neutrino (from MWTC) with m < 800 GeV is excluded • Majorana neutrino with m > 100 GeV candidate for dark matter: not excluded by direct searches • In standard expansion case from flavor mixed Majorana mass term • Mainly sterile Majorana neutrino with m > 23 GeV candidate for dark matter: not excluded by LEP or direct searches. • Further studies: • Updating our different neutrino mixing results • Other CDM (adjoint fermions) in extensions of MWTC • Replacing Quintessence with more advanced DE models
