Neutrinos and Particle Physics Models. Pierre Ramond Institute for Fundamental Theory University of Florida

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1 Neutrinos and Particle Physics Models Pierre Ramond Institute for Fundamental Theory University of Florida

2 Editorial Early History Neutrino masses Neutrinos & Yukawa Unification

3 Neutrino revealed by pure thought to save a fundamental principle NOT by direct measurement and treated with suspicion by most physicists YET

4 Neutrinos never quite fit current dogma Left-handed in an ambidextrous world parity violation Massless because of new symmetries? (Volkov-Akulov, Fayet) Absurdly light: sign of a new scale? Large neutrino mixings CP violation Leptogenesis Matter Asymmetry Keys to Yukawa Unification?

5 Sun Messengers from the Universe Supernovas Blazers Neutrino Masses & Mixings: Only Physics Beyond the Standard Model a small portion of physicists works on neutrinos but not all ignored neutrinos

6 obels E. Fermi 1938 W. Pauli 1945 L. Lederman 1988 M. Schwartz 1988 J. Steinberger 1988

7 obels F. Reines 1995 R. Davis 2002 M. Koshiba 2002 T. Kajita 2015 A. McDonald 2015

8 hall of fame E. Majorana B. Pontecorvo M. Goldhaber S. Sakata J. Bahcall L. Wolfenstein

9 Early History

Zurich, December 4, 1930 Dear Radioactive Ladies and Gentlemen: I have hit upon a desperate remedy to save the exchange theorem of statistics and the energy theorem.

10 Zurich, December 4, 1930 Dear Radioactive Ladies and Gentlemen: I have hit upon a desperate remedy to save the exchange theorem of statistics and the energy theorem. there could exist in the nuclei electrically neutral particles which have spin ½, and do not travel with the velocity of light. The continuous beta spectrum would then become understandable. I do not feel secure enough to publish anything about this idea only those who wager can win. Unfortunately, I cannot personally appear in Tübingen, since I am indispensable here on account of a ball

11 Pauli at Pasadena meeting June 1931: my little neutron is bound in the nucleus Pauli divorces actress Kate Depner Pauli under analysis with C. Jung Two years later Chadwick discovers the Neutron Nitrogen problem solved Fermi: Pauli s little neutron is a free particle, the neutrino

12 1936: Bethe-Bacher (Rev Mod Phys) 1938: neutrino n renamed ν by E.M. Lyman 1948: H. R. Crane (Rev Mod Phys)

13 : Cowan and Reines Project Poltergeist Detection of the free neutrino Phys Rev 92,830 (1953) Status of an experiment to detect the free neutrino invited talk at January 1954 APS meeting Detection of the free neutrino: a confirmation Nature, 124,3212 (1956)

14 1937 E. Majorana (Il Nuovo Cimento 14, 171) 1939 W. Furry (Phys Rev 56, 1184) applies Majorana neutrino to ββ 0ν decay

15 1945: Pontecorvo (Chalk River preprint) e + 37 Cl! 37 Ar + e nice but not practical (Fermi) 1957: R Davis designs pilot experiment at the Savanah River reactor to detect neutrinos!

16 B. Pontecorvo ( J. Exptl. Theoret. Phys. (U.S.S.R.) 33, 549 (1957) neutrino-antineutrino transitions (oscillations)

17 1962: Maki Nakagawa Sakata (Prog Theo Phys 28, 870) flavor mixing and flavor transitions (oscillations)

18 Neutrino masses

19 theorists weigh in extreme kinematics (Fermi ) absurdly light neutrinos beyond the Standard Model light Standard Model Neutrinos L i = e e i ē j H (BEH boson)

20 New Leptonic BEHs L [i L j] isosinglet S ` =2 fermion bilinears L (i L j) isotriplet T ` =2 (type II) ē i ē j isosinglet S ++ ` = 2 New Fermions (L i H)0 isosinglet neutrinos N j (type I) (L i H)1 isotriplet leptons j (type III)

21 physics of scalar extensions determined by potential µ(hh) 1 T (type II) cubic terms ` =2 µ 0 S ++ S S µ 00 S ++ (TT) 0 µ 000 S + S + (TT) 0 total lepton number broken at μ-scales quartic terms ` =0

22 loop level mass models simplest add extra BEH boson H 0 µ(h 0 H) 0 S + flavor-antisymmetric coupling L [i L j] S + (Zee; Babu; Ma; Gustafsson, No, Rivera; ) (Type I: Minkowski;Yanagida; Gell-Mann, Ramond, Slansky; Glashow) (Type II: Konetschny, Kummer; Cheng, Li; Lazarides, Shafi, Wetterich; Schecter, Valle; Mohapatra et al,; Ma;... ) (Type III: Foot, He, Joshi; Ma; )

23 A Winning Combination: Dirac and Majorana Dirac mass m (L H) 0 N ` =0 Majorana mass M N N ` =2 Suppression m M EW GUT 1 I w = 1 2 I w =0 m = m m M Natural GUT Scale SU 5, SO 10, E 6,

24 Neutrino Phases and Mixings link Electroweak to GUT physics U PMNS = U 1 U Seesaw U 1 diagonalizes charged lepton Yukawas: I w = 1 2 physics U Seesaw diagonalizes the seesaw: I w =0 physics symbolically expt Seesaw + EW EW Seesaw Cabibbo Haze angles less than CKM s from I w =0 physics

25 Masses oscillations 2 12 m 2 1 m 2 2 =(8.68 mev ) m 2 1 m 2 3 = (49.40 mev ) 2 m 3 m 2 m 1 cosmology m 1 + m 2 + m 3 apple 0.22 ev

26 Angles reactor angle 13 =8.37 ±.16 < Cabibbo neutrino surprise: two large angles atmospheric 23 = I w =0 physics solar 12 = 33.6 ± 0.8 ` =0 ` =2 one Dirac phase two Majorana phases solar and atmospheric angles mostly from Seesaw reactor angle from either EW and/or Seesaw

27 Neutrinos & Yukawa Unification

28 Dirac s Path Seek Simplicity and Beauty in gauge couplings in Yukawa couplings

29 Tension in the Yukawa Sector At GUT scale, quark and neutrino gauge couplings unify disparate Yukawa couplings small quark mixing angles < 13 0 neutrino surprise! two large neutrino mixing angles

30 Majorana Crystal at GUT scale Discrete Family Symmetry at GUT scale (Pakvasa, Sugawara; Ma; 10 3 more authors ) three chiral families discrete SU 3, SU 2 subgroups SU 2 : A4 double cover, SU 3 : Δ 27,, T 7, PSL(2,7)

31 Grand Unification Primer Yukawa Couplings u d e

32 Grand Unification Primer Yukawa Couplings u d e D

33 Grand Unification Primer Yukawa Couplings u d e D Majorana mass M

34 CKM d u e

35 CKM d u e D

36 CKM d u e D

37 CKM d SU 5 u e D

38 CKM d SU 5 u e D

39 CKM d SU 5 u e SO 10 D

40 CKM d SU 5 u e SO 10 D M

41 CKM d SU 5 u e SO 10 D M

42 CKM d SU 5 u e SO 10 PMNS D M

43 Seesaw Simplicity small angle all from Cabibbo Haze two large angles only from Seesaw Tri-Bi-Maximal Matrix pretty matrix with an ugly name (L. Everett) U Seesaw = p p 1 p 2/3 p 1/3 p 0 p 1/6 p 1/3 1/2 A p 1/6 1/3 1/2

44 simplest SO 10 Y 2/3 = Y D = A correlated hierarchy Majorana mass A M = M A M 0 inverse eigenvalues = neutrino masses

45 M 0 TBM diagonalization: relations among its elements (12)=(13); (22)=(33); (23) (22) = (11) (12) PSL(2,7) coupling (22) = (23); m 1 m 2 = 1 2 m 3 50 mev, m 2 11 mev, m mev BUT TBM Mixing requires asymmetric Yukawa Matrices (J. Kile, J. M. Pérez, PR, J. Zhang, 2014)

46 SU 5 Yukawas (M. H. Rahat, PR, B. Xu, 2018) Y 5 Y 45 : : p A p A 2 3A p A A A + 2 3A A A, ρ, η, λ Wolfenstein parameters satisfies CKM, Gatto & Gut-scale Georgi-Jarlskog relations r md m s m b = m ; m µ =3m s ; m d =3m e PMNS angles o above pdg 2.9 o below pdg 6.16 o above pdg

47 Phase in TBM matrix reduces 13 cos =0.2 brings 13 to its pdf value PMNS angles at pdg 0.66 o below pdg 0.51 o above pdg Jarlskog-Greenberg invariant J = CP = 8 < 1.32 : - sign sign

48 neutrino detectors

49 The Sun Never Sets on neutrino detectors

50 A Prediction

51 Neutrino Chronology Revelation (13) yrs later Detection (17) yrs later Oscillations 1998

52 Neutrino Chronology Revelation (13) yrs later Detection (17) yrs later Oscillations (19) yrs later

53 Neutrino Chronology Revelation (13) yrs later Detection (17) yrs later Oscillations (19) yrs later 2052! decay ββ0ν

Neutrino Chronology Revelation 1930 2(13) yrs later Detection 1956 2 2 (17) yrs later Oscillations

54 Neutrino Chronology Revelation (13) yrs later Detection (17) yrs later Oscillations (19) yrs later ββ0ν decay 2052! longevity required neutrinos prospecting should be a family affair

NEUTRINOS. Concha Gonzalez-Garcia. San Feliu, June (Stony Brook-USA and IFIC-Valencia)

NEUTRINOS. Concha Gonzalez-Garcia. San Feliu, June (Stony Brook-USA and IFIC-Valencia) NEUTRINOS (Stony Brook-USA and IFIC-Valencia San Feliu, June 2004 Plan of Lectures I. Standard Neutrino Properties and Mass Terms (Beyond Standard II. Neutrino Oscillations III. The Data and Its Interpretation