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Models and Non Standard Model with Neutrinos

Models and Non Standard Model with Neutrinos . Pilar Hernández University of Valencia/IFIC. SM + massive n s. Fogli et al 2012 (after T2K, Double-CHOOZ, Daya Bay, RENO ). 3 n mixing:. Standard 3 n scenario. The flavour observables:. Good prospects for CP volation.

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Models and Non Standard Model with Neutrinos

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  1. Models and Non Standard Model with Neutrinos Pilar Hernández University of Valencia/IFIC

  2. SM + massive ns Fogli et al 2012 (after T2K, Double-CHOOZ, Daya Bay, RENO) 3nmixing:

  3. Standard 3n scenario The flavour observables:

  4. Goodprospectsfor CP volation Coloma, Donini, Fernandez-Martinez,PH arXiv:1203.5651

  5. New dofs puzzle Neutrinos are massive -> there must be new dofs in the SM

  6. New dofs puzzle Neutrinos are massive -> there must be new dofs in the SM Weinberg

  7. SM ? nSM

  8. The good nSM • Explanation for the neutrino-charged lepton hierarchy

  9. Thenflavour puzzle I Why are neutrino masses so light ?

  10. The good nSM • Explanation for the neutrino-charged lepton hierarchy • Explain the pattern of mixing

  11. Thenflavour puzzle II CKM VCKM = PDG 2007 PMNS Gonzalez-Garcia, Maltoni Differences are striking!

  12. The good nSM • Explanation for the neutrino-charged lepton hierarchy • Explain the pattern of mixing • Explain other open problems: DM, matter-antimatter, oscillation anomalies, cosmology anomalies…

  13. Massive Neutrinos & fundamental questions in Particle Physics and Cosmology Structure of the vacuum ? DE ? DM ? Baryons ? Flavour Puzzle: twice as many pieces ? Growth of structure

  14. Outlier I: LSND anomaly LSND vs KARMEN Appearance signal with very different - Not yet disproved at an acceptable level of confidence…

  15. Pinning down the New physics scale Hierarchy problem or SUSY ? eV keV MeV GeV TeV meV Leptogenesis SUSY GUTs

  16. Pinning down the New physics scale bb0n LFV processes, Precision tests, LHC Neutrino osc. Hierarchy problem or SUSY ? eV keV MeV GeV TeV meV CMB, LSS Baryogenesis Leptogenesis SUSY GUTs Nucleosynthesis

  17. The good nSM • Explanation for the neutrino-charged lepton hierarchy • Explain the pattern of mixing • Explain other open problems: DM, matter-antimatter, oscillation anomalies, cosmology anomalies… • Do so, in a predictable and testable way !

  18. No signal of SUSY/solution-of-hierarchy-problem at the LHC (yet)…

  19. Occam’s razor

  20. Pinning down the New physics scale 2) LHC reach 3) LSND reach 1) Decoupling physics Warm DM ? Hierarchy ? eV keV MeV GeV TeV meV LSND, reactor anomalies? Extra radiation ? Matter/antimatter asymmetry ? GUT ? Ruchayskiy’s talk

  21. Effective Theories of Neutrino Masses(model-independent) IfL >> vlow-energyeffectsshould be welldescribed by aneffectivefieldtheory: Weinberg; Buchmuller, Wyler;… Oidbuiltfrom SM fieldssatisfyingthegaugesymmetries Onlyonewithd=5: Weinberg’soperatoror neutrino masses ! Genericallyd=6 operators: richphenomenology

  22. d=6 phenomenology Long listofflavoured-operators • rareleptondecays: m -> e g • Z, W decays • rhoparameter • W mass, … • violationsofuniversality, unitarity,… But…

  23. la -> lbg MEG Ifjust neutrino masses: Ifalsod=6 operators@oneloop

  24. Could d=6 be stronger ? Yesiftwoindependentscales in d=5, d=6 from a symmetryprinciple: leptonnumber Cirigliano et al 05, Kersten,Smirnov 07 ; Abada et al 07 • Ld=5~LLN>> Ld=6 ~ LLFV~ TeV • Originoflepton/quarkflavourviolationlinkedtotheLEW • Lepton number breaking scale higher and responsible • for the gap between n and remaining fermions

  25. Are d=6 flavour structures related to neutrino masses ? Minimal Flavour Violation Chivukula, Georgi; Buras et al.;D’Ambrosio et al; Cirigliano et al; Davidson et al, Gavela, et al (cd=5)ab~(cd=6)ab~mn All flavour violating effects determined by neutrino masses and mixings Unfortunately not the case for most popular models of neutrino mass (ex. Type I seesaw)

  26. BSM and Neutrino Masses(Up->Down approach) ?

  27. New physics scale Type I see-saw: interchange a heavysingletfermion Minkowski; Gell-Mann, RamondSlansky; Yanagida, Glashow…

  28. New physics scale Type II see-saw: interchange a heavy triplet scalar Konetschny, Kummer; Cheng, Li; Lazarides, Shafi, Wetterich…

  29. New physics scale Type III see-saw: interchange a heavy triplet fermion Foot et al; Ma; Bajc, Senjanovic…

  30. New physics scale Alsofromloops ! Zee-Babu Systematicexplorationof 1-loopgenerated Weinberg interaction Bonnet et al 2012

  31. Effectivesee-sawtheories Alsod=6operators Type I Non-unitarity in mixing ! Type III Type II Gavela, Broncano, Jenkins; Abada, et al

  32. Type I Seesaw Most general (renormalizable) Lagrangian compatible with SM gauge symmetries: Y: 3 xnRMN: nRxnR mn ms

  33. Onescalesee-sawmodels Ye

  34. Type I or III + (approx) Lepton number Wyler, Wolfenstein; Mohapatra, Valle; Branco, Grimus, Lavoura, Malinsky, Romao,… nR Inverse Seesaw Direct Seesaw L= +1 -1 +1 mn mn v MN/m M2N/m Y unsuppressed: -> LFV effects at LHC, large m-> eg, etc -> heavier spectrum MN,Yv Kersten,Smirnov 07; Abada et al 07; Gavela,et al 09

  35. MinimalFlavour type I seesaw model Gavela, Hambye, Hernandez, PH 09 Only two extra Weyl fermions + SM Y, Y’ complex vectors, L, m, m’ numbers

  36. Minimal type I seesaw model Neutrino masses & mixings determine Y up to a global normalization (and Majorana phase) Normal hierarchy Inverted hierarchy AlsoRaidal, Strumia, Turzynski 2004; Ibarra et al 2010

  37. Complementarityof CLFV and neutrino oscillations NH IH Gavela, Hambye, Hernandez, PH 09

  38. CLFV within reach Dinh, Ibarra, Molinaro, Petcov 2012

  39. LLFV ~ TeV: directsearches at LHC ? Keung, Senjanovic;… • Generically it is needed • Gauge interactions of extra fields for large enough production • (ex. type II and type III) • Low enough masses for kinematical constraints Type II: Han et al;Garayoa, Schwetz; Kadastik,et al ; Akeroyd, et al; Fileviez et al, del Aguila et al Type III: Franceschini et al; Arhrib et al; Eboli et al…

  40. MinimalFlavourSee-sawIII at LHC Eboli, Gonzalez-Fraile, Gonzalez-Garcia 2011

  41. CMS-PAS-HIG-12-005 Type II seesaw

  42. LSND anomaly In order to accommodate a new • Need at least four (ns ≥1) distinct eigenstates • Apparently CP violating effect needed (signal LSND/MB anti-n not MB n) • ns ≥ 2 • Tension appearance (signal) and disappearance (no signal) ? • Tension with cosmology ?

  43. Outlier II: reactor anomaly old fluxes underestimated by 3%: Re-calculation of reactor fluxes: Mueller et al, ArXiv: 1101.2663

  44. Outlier III: Cosmology Hamann et al, ArXiv: 1006.5276 Sterile species favoured by LSS and CMB Nucleosynthesis: Izotov, Thuan

  45. 3+2 neutrino mixing model Parametrized in terms of a general unitary 5x5 mixing matrix (9 angles, >6 phases physical) Kopp, Maltoni, Schwetz (KMS) arXiv:1103.4570 Giunti, Laveder, (GL) arXiv:1107.1452 Significant improvement over 3n scenario, but tension appearance/disappearance remains

  46. Pheno 3+ns mixing models ? Assumes a general mass matrix for 3+ns neutrinos: what is that model ? 3xns 3x3

  47. Pheno 3+ns mixing models ? Assumes a general mass matrix for 3+ns neutrinos: Gauge invariance Effective theory: MLLparametrizes our ignorance about the underlying dynamics (eg. a model with nR > ns, where the heavier states are integrated out)

  48. Type I see-sawmodels Light sterile states! De Gouvea, hep-ph/0501039 De Gouvea, J. Jenkins, Vasudevan hep-ph/0608147

  49. Minimal models Most general (renormalizable) Lagrangian compatible with SM gauge symmetries: 3+2 minimal much more predictive than 3+2 pheno Donini, PH, Lopez-Pavon, Maltoni 2011; De Gouvea et al 2011;

  50. Heavy-Light Mixings Heavy-light mixings are predicted up to a complex angle z45 and two CP phases ! Normal Hierarchy and Suppressed in Suppressed only in Inverse Hierarchy

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