1. Neutrino Masses and the Quest for Unification K.S. Babu Oklahoma State University Physics Seminar Wichita State University, Wichita, KS November 6, 2013

2. Cosmic Gall Neutrinos, they are very small. They have no charge and have no mass And do not interact at all. The earth is just a silly ball To them, through which they simply pass, Like dustmaids down a drafty hall Or photons through a sheet of glass. They snub the most exquisite gas, Ignore the most substantial wall, Cold-shoulder steel and sounding brass, Insult the stallion in his stall. And, scorning barriers of class, Infiltrate you and me! Like tall And painless guillotines, they fall Down through our heads into the grass. At night, they enter at Nepal And pierce the lover and his lass From underneath the bed—you call It wonderful; I call it crass. John Updike Telephone Poles and Other Poems, 1963

5. Postulated by Pauli as a desperate measure to restore momentum and energy conservation in beta decay (1930) Electron type neutrino discovered by Reines and Cowan in reactor experiments (1956) -- Nobel Prize in 1995 Muon type neutrino produced in accelerators by Lederman, Schwartz, Steinberger et al (1962) – Nobel Prize in 1988 LEP experiments measure N(nu) = 2.994 +-0.012 (1991-2002) Neutrinos from the Sun detected by Davis et al (1968) – Nobel Prize in 2002 Neutrinos from Supernova 1987A detected in US and Japan -- Koshiba, Nobel Prize in 2002 Neutrino oscillations discovered in atmospheric neutrinos [IMB, Kamiokonde Hints (1988), Discovery by SuperKamiokande (1998)] Solar neutrino deficit confirmed by various experiments and interpreted as evidence for neutrino oscillations (1968 –) Reactor antineutrino oscillations discovered – Daya Bay (2012), RENO, DoubleChooz, T2K A Brief History of Neutrinos

6. Neutrinos from the Sun

9. Neutrinos from the sky

11. L/E Dependence of atmospheric neutrinos

12. Daya Bay Reactor Neutrino Experiment

13. Global Fit to 3-Neutrino Oscilaltions

15. Minkowski (1977) Yanagida (1979) Gell-Mann, Ramond, Slansky (1979) Mohapatra, Senjanovic (1980)

16. Leptons Quarks Disparity a challenge for Quark-Lepton unified theories. Neutrino mixing versus quark mixing

17. Neutrino Masses Probe the Scale of Unification of all Forces

18. The Greatest Equations Ever?

19. Tied for 1 st place:

20. Top Finishers

21. Quantum Mechanics & Relativity Dirac’s Equation (1927)

22. Antiparticles

23. Quantum Electrodynamics

24. Great Success of Quantum Electrodynamics e  e e   e+e-→+-e+e-→+-

26. + - - - - - - + + + + + R + Test charge -

27. +- R - - - - - - + + + + + +

30. q g g g g g

31. Causes charge screening

32. Causes color charge anti-screening

34. Gross, Wilczek, Politzer Nobel Prize, 2004 Asymptotic freedom

38. d dduddu uu d e,, W ±, Z 0 e,  Energy 1 GeV10 2 GeV 10 16 GeV 10 19 GeV

41. With SUSY, Quadratic Divergence Cancels

42. SM Particles SUSY Partners Spin = 1/2 Spin = 0 Spin = 1/2 Spin = 1 Spin = 1/2

43. More Hints in favor of GUTs

46. Standard Model SO(10) Structure of Matter Multiplets

50. Baryon asymmetry of the universe

52. Sakai, Yanagida (1982) Weinberg (1982)

53. (Dimopoulos-Wilczek mechanism) Proton Decay in Supersymmetric SO(10) Dimopoulos, Wilczek (1981) Babu, Barr (1993) Barr, Raby (2000) Babu, Pati, Wilczek (2000) Babu, Pati, Tavartkiladze (2010)

54. Gauge coupling evolution in explicit SO(10) model

55. Correlation between two modes of proton decay

56. Proton lifetime expectations

57. Model has only 11 real parameters plus 7 phases Minimal SO(10) Model Babu, Mohapatra (1993) Fukuyama, Okada (2002) Bajc, Melfo, Senjanovic, Vissani (2004) Fukuyama, Ilakovac, Kikuchi, Meljanac, Okada (2004) Aulakh et al (2004) Bertolini, Frigerio, Malinsky (2004) Babu, Macesanu (2005) Bertolini, Malinsky, Schwetz (2006) Dutta, Mimura, Mohapatra (2007) Bajc, Dorsner, Nemevsek (2009)

58. FitInput at GUT scale Output: Type II Seesaw Babu, Macesanu (2005) Specific Example for Quark & Lepton masses

59. Theta(13) in Minimal SO(10)

60. Summary and Conclusions

61. Acknowledgments