Neutrinos and Particle Physics Modelsneutrinohistory2018.in2p3.fr/talks/03_Ramond.pdf ·...
Transcript of Neutrinos and Particle Physics Modelsneutrinohistory2018.in2p3.fr/talks/03_Ramond.pdf ·...
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Neutrinos and Particle Physics Models
Pierre Ramond Institute for Fundamental Theory
University of Florida
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Early History
Neutrino masses
Neutrinos & Yukawa Unification
Editorial
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revealed by pure thought
to save a fundamental principle
Neutrino
and treated with suspicion by most physicists
NOT by direct measurement
YET …
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Left-handed in an ambidextrous world parity violation
Absurdly light: sign of a new scale?
Matter AsymmetryLeptogenesis
Keys to Yukawa Unification?
Massless because of new symmetries?
CP violation
(Volkov-Akulov, Fayet)
Neutrinos never quite fit current dogma
Large neutrino mixings
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Messengers from the Universe Supernovas
Neutrino Masses & Mixings:
Only Physics Beyond the Standard Model
a small portion of physicists works on neutrinos
Sun
Blazers
but not all ignored neutrinos
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W. PauliE. Fermi19451938
obels⌫
L. Lederman1988
M. Schwartz1988
J. Steinberger1988
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F. Reines1995
R. Davis2002
M. Koshiba2002
2015A. McDonaldT. Kajita
2015
obels⌫
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B. Pontecorvo M. Goldhaber
hall of fame⌫
J. Bahcall L. Wolfenstein
E. Majorana
S. Sakata
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Early History
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“ 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…
Zurich, December 4, 1930
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Two years later
Pauli under analysis with C. Jung
Pauli at Pasadena meeting June 1931: my little neutron is bound in the nucleus
1933-1934 Fermi: Pauli’s little neutron is a free particle, the “neutrino”
Chadwick discovers the Neutron Nitrogen problem solved
Pauli divorces actress Kate Depner
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1936: Bethe-Bacher (Rev Mod Phys)
1938: neutrino “n” renamed ν by E.M. Lyman
1948: H. R. Crane (Rev Mod Phys)
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1953-1956: Cowan and Reines
“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)
Project Poltergeist
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1939 W. Furry (Phys Rev 56, 1184)
1937 E. Majorana (Il Nuovo Cimento 14, 171)
applies Majorana neutrino to ββ0ν decay
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1945: Pontecorvo (Chalk River preprint)
⌫e + 37Cl ! 37Ar + e�
“nice but not practical” (Fermi)
1957: R Davis designs pilot experiment at the Savanah River reactor to detect neutrinos!
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B. Pontecorvo ( J. Exptl. Theoret. Phys. (U.S.S.R.) 33, 549 (1957)
neutrino-antineutrino transitions (oscillations)
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flavor mixing and flavor transitions (oscillations)
1962: Maki Nakagawa Sakata (Prog Theo Phys 28, 870)
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Neutrino masses
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absurdly light neutrinos
extreme kinematics
(Fermi 1933-34)
theorists weigh in
Li =
✓⌫ee�
◆
iHej
Standard Model Neutrinos
(BEH boson)
“beyond the Standard Model” light
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isosinglet
isotripletL(iLj)
L[iLj]
eiej
isosinglet neutrinos
fermion bilinears
isosinglet
T ` = 2
S� ` = 2
S++ ` = �2
New Leptonic BEHs
New FermionsNj
isotriplet leptons ⌃j
(LiH)0
(LiH)1
(type I)
(type III)
(type II)
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physics of scalar extensions determined by potential
cubic terms
quartic terms
µ0 S++S�S�
|�` = 2|
|�` = 0|
µ000S+S+(T T )0
µ00S++(T T )0
µ(HH)1T
total lepton number broken at μ-scales
(type II)
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loop level mass models
simplest add extra BEH boson H 0 µ(H 0H)0S+
flavor-antisymmetric coupling L[iLj] S+
(Zee; Babu; Ma; Gustafsson, No, Rivera;…)
(Type II: Konetschny, Kummer; Cheng, Li; Lazarides, Shafi, Wetterich; Schecter, Valle; Mohapatra et al,; Ma;... )
(Type I: Minkowski;Yanagida; Gell-Mann, Ramond, Slansky; Glashow)
(Type III: Foot, He, Joshi; Ma;…)
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Majorana mass
Dirac mass
A Winning Combination: Dirac and Majorana
N
(LH)0 |�` = 0|
|�` = 2|
�Iw = 12
�Iw = 0
m
M
m
M
·N
·N
⇠ ⌧ 1EW
GUT Suppression ⇠
m⌫ = mm
M
Natural GUT Scale SU5, SO10, E6, · · ·
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Neutrino Phases and Mixings
UPMNS = U†�1 USeesaw
symbolically
U�1 diagonalizes charged lepton Yukawas: �Iw =1
2physics
link Electroweak to GUT physics
�Iw = 0USeesaw diagonalizes the seesaw: physics
✓EW
✓Seesaw
✓expt
⇡ ✓Seesaw
“ + ” ✓EW
“Cabibbo Haze” angles less than CKM’s
from �Iw = 0 physics
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m⌫1 +m⌫2 +m⌫3 0.22 eVcosmology
Masses
m⌫1
m⌫2
m⌫3
�212 ⌘ |m2
⌫1�m2
⌫2| = (8.68 meV )2
�213 ⌘ |m2
⌫1�m2
⌫3| = (49.40 meV )2
oscillations
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Angles
two large angles
one Dirac phasetwo Majorana phases
neutrino surprise:
atmospheric
solar
�` = 0
�` = 2
reactor angle ✓13 = 8.37� ± .16� < ✓Cabibbo
✓23 = 40.2�+1.4�
�1.6�
✓12 = 33.6� ± 0.8�physics�Iw = 0
reactor angle from either and/or ✓EW ✓Seesaw
solar and atmospheric angles mostly from ✓Seesaw
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Neutrinos & Yukawa Unification
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in gauge couplings
in Yukawa couplings
Dirac’s Path
Seek Simplicity and Beauty
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disparate Yukawa couplings
small quark mixing angles < 130
two large neutrino mixing angles
At GUT scale, quark and neutrino
Tension in the Yukawa Sector
gauge couplings unify
neutrino surprise!
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Majorana Crystal at GUT scale
(Pakvasa, Sugawara; Ma; 103 more authors …)
Discrete Family Symmetry at GUT scale
three chiral families discrete SU3, SU2 subgroups
SU2 : A4 double cover, …
SU3 : Δ27, … , T7, PSL(2,7)
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u d e
Yukawa Couplings
Grand Unification Primer
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u d e ⌫D
Yukawa Couplings
Grand Unification Primer
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u d e ⌫D
Yukawa Couplings
M
Majorana mass
Grand Unification Primer
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u
d
e
CKM
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u
d
e
⌫D
CKM
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u
d
e
⌫D
CKM
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u
d
e
⌫D
SU5CKM
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u
d
e
⌫D
SU5CKM
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u
d
e
⌫D
SU5
SO10
CKM
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u
d
e
⌫D
SU5
SO10
CKM
⌫
M
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u
d
e
⌫D
SU5
SO10
CKM
⌫
M
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u
d
e
⌫D
SU5
SO10
CKM
PMNS
⌫
M
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two large angles
all from “Cabibbo Haze” small angle
only from Seesaw
“pretty matrix with an ugly name” (L. Everett)
Tri-Bi-Maximal Matrix
Seesaw Simplicity
“pretty matrix with an ugly name” (L. Everett)
USeesaw =
0
@
p2/3
p1/3 0
�p1/6
p1/3
p1/2p
1/6 �p
1/3p
1/2
1
A
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0
@✏4 00 ✏2 00 0 1
1
A
simplest SO10
Y 2/3 = Y ⌫D =
correlated hierarchy
0
@✏4 00 ✏2 00 0 1
1
A
0
@✏4 00 ✏2 00 0 1
1
A
M = M0Majorana mass
M0 inverse eigenvalues = neutrino masses
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m⌫3⇠ 50 meV, m⌫2
⇠ 11 meV, m⌫1⇠ 5.5 meV
TBM diagonalization: M0 relations among its elements
(12)=(13); (22)=(33); (23) − (22) = − (11) − (12)
PSL(2,7) coupling (22) = (23); |m⌫1
m⌫2
| = 1
2
BUT
TBM Mixing requires asymmetric Yukawa Matrices
(J. Kile, J. M. Pérez, PR, J. Zhang, 2014)
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1
3
0
@2p
⇢2 + ⌘2�4 �3 3Ap⇢2 + ⌘2�3
�3 0 3A�2
3Ap
⇢2 + ⌘2�3 3A�2 3
1
A +2
3A
0
@0 0 00 0 01 0 0
1
A
1
3
0
@0 0 00 �2 00 0 0
1
A
Y 5
Y 45
SU5 Yukawas
satisfies CKM, Gatto & Gut-scale Georgi-Jarlskog relations
A, ρ, η, λ Wolfenstein parameters
� ⇡r
md
msmb = m⌧ ; mµ = 3ms; md = 3me
:
:
(M. H. Rahat, PR, B. Xu, 2018)
PMNS angles✓13
✓12
✓23
2.26o above pdg
2.9o below pdg
6.16o above pdg
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Phase in TBM matrix reduces
brings to its pdf value✓13cos� = 0.2
✓13�
PMNS angles✓13
✓12
✓23
at pdg
0.66o below pdg
0.51o above pdg
Jarlskog-Greenberg invariant J = |0.027|
- sign�CP =
8<
:
1.32⇡
0.67⇡ + sign
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neutrino detectors
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The Sun Never Sets
on neutrino detectors
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A Prediction
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Neutrino Chronology Revelation 1930
Detection 1956
Oscillations 199822(17)
yrs later2(13)
yrs later
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Neutrino Chronology Revelation 1930
Detection 1956
Oscillations 199822(17)
yrs later2(13)
yrs later
23(19) yrs later
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Neutrino Chronology Revelation 1930
Detection 1956
Oscillations 199822(17)
yrs later2(13)
yrs later
23(19) yrs later 2052! decayββ0ν
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Neutrino Chronology Revelation 1930
Detection 1956
Oscillations 199822(17)
yrs later2(13)
yrs later
23(19) yrs later
longevity required
neutrinos prospecting should
be a family affair
2052! decayββ0ν