Page 1
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Neutrino Theory: Mass, Interactions,Unification
Oleg PopovSeoul National University of Science and Technology
[email protected]
IBS, 6.03.2019
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Page 2
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Overview
1 Introduction
2 Tree level
3 Radiative
4 Dirac case
5 B-L extension
6 Unification
7 Connection to GW
8 Summary
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Page 3
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Introduction/Motivation
(Naturally) small neutrino masses
Connection with dark matter existence
Lepton mixing
Unification
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Page 4
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Standard Model
Gauge symmetry group GSM = SU(3)c × SU(2)L × U(1)Y
LY = uYuQH + QYddH + h.c. (1)⟨h0⟩
= v → mf = Yf v (2)
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Page 5
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Requirements for neutrino mass
Majorana or Dirac type?
Tree level or radiative?
New particles? (scalar, fermionic, vector)
New gauge sectors? (U(1), SU(2),SU(N))
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Page 6
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Possible effects/ Ways to test
Collider (LHC,ILC, FCC)
Dark matter
Grand unified theories
Neutrino mixing
Leptogenesis (CPV)
Neutrinoless N−pole beta decay(0νnβ)
GW via scalar sector
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NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Tree level, Majorana
Weinberg Operator 1979: LHLHΛ = (l−H+−νH0)(l−H+−νH0)
ΛAdd NR ∼ (1, 1, 0) under GSM
Lnew = NYDLH + mNNRNR + h.c.
v � mN ∼ 1011GeV → mν � v with YD ∼ 1or YD � 1→ mν � v with mN ∼ O(102−3GeV )
Seesaw−I
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NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Seesaw-I
Add[1980] ξ = (ξ++, ξ+, ξ0) ∼ (1, 3, 1) under GSM
Lnew = YLξL + h.c.− µHξH → mν = Y⟨ξ0⟩
= −2Yµv2
Mξ
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Page 9
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Seesaw-III
Weinberg Operator 1979: LHLHΛ = (l−H+−νH0)(l−H+−νH0)
ΛAdd NR ∼ (1, 1, 0) under GSM
Lnew = ΣYDLH + mNΣRΣR + h.c.
v � mN ∼ 1011GeV → mν � v with YD ∼ 1or YD � 1→ mν � v with mN ∼ O(102−3GeV )
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Page 10
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Seesaw variations
Seesaw[1979] mν = −m2D/mN
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NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Seesaw variations
Inverse Seesaw[1986] mν = m2Dm2/(m2
N −m1m2)
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Page 12
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Seesaw variations
Linear Seesaw mν = −2mDmD′/mN
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Page 13
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Radiative neutrino mass, Majorana
Zee[1986]
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NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Radiative neutrino mass, Majorana
Ma[2006]
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Page 15
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Scotogenic radiative neutrino mass
Add Z2 symmetry under which η ∼ (1, 2, 1/2) and NR are ood
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NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Radiative neutrino mass, Majorana
Fraser,Ma,OP[2014]
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Page 17
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Radiative inverse seesaw neutrino mass, Majorana
Add Z2 symmetry under which real singlet scalar andEL,R ∼ (1, 2, 1/2) and NL ∼ (1, 1, 0) are odd
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Page 18
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Dirac neutrinos
Add NR ∼ (1, 1, 0) under GSM
NR MUST transfor under some other symmetrynon-trivially
New symmetry S is discrete, global, gauged, dark?
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Page 19
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Tree Dirac case
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Page 20
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Dirac case
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Page 21
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Dirac case
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Page 22
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
U(1)B−Lcase
Add 3 NR ∼ (1, 1, 0) which carry L = (1, 1, 1)
Add 3 NR ∼ (1, 1, 0) which carry L = (4, 4,−5)
Other variations are possible
Makes U(1)B−L anomaly free.
U(1)B−L can global or gauged
Global: softly or spontaneously broken(Majorana, Dirac)
Gauged: spontaneously broken(Majorana, Dirac)
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Page 23
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Scotogenic model in SU(6) GUT∗
Simple case: Extend SU(5) to SU(6) to incude BSM particlesneeded5∗F × 10F × 5∗S , 10F × 10F × 5S SU(5) Yukawa terms areextended to6∗F × 15F × 6∗S , 15F × 15F × 15S SU(6) YukawasAnomaly free combinations: 5∗F + 10F for SU(5),6∗F + 6∗F + 15F for SU(6). New SU(6) 21S scalar is added toobtain 2’nd Higgs doublet (Z2 ∼ −) with new interactions6∗F × 6∗F × 21S , 15∗S × 15∗S × 21S × 21S
∗10.1088/1742-6596/539/1/01200122/26
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NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Scotogenic model in SU(7) GUT†
Less simple case: Extend SU(5) to SU(7) to incude BSMparticles needed5∗F × 10F × 5∗S , 10F × 10F × 5S SU(5) Yukawa terms areextended to7∗F × 21F × 7∗S , 21F × 21F × 35S SU(7) YukawasAnomaly free combination for SU(7): 7∗F + 7∗F + 7∗F + 21F .New 28S scalar needed to accomodate SU(2)N doublet, withnew interactions:7∗F × 7∗F × 28S , 21∗S × 21∗S × 28S × 28S
†10.1088/1742-6596/539/1/012001
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NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Connection to GW signals
Neutrino mass requires new scalars or gauge bosons
Strong first order phase transition (BSM gauge symmetry)
Strong first order phase transition gives GW
Some possible models: LR models, SU(N) scotognicsymmetry
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Page 26
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Leptogenesis
25/26
Page 27
NeutrinoTheory
Introduction
Tree level
Radiative
Dirac case
B-L extension
Unification
Connection toGW
Summary
Summary
Neutrino masses can be Majorana or Dirac
Tree or radiative
Reuire BSM fields and symmetries (globa or gauged)
Connection with DM
Connection with GW
Leptogenesis
Thank you!
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