Models and non standard model with neutrinos
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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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Models and Non Standard Model with Neutrinos

Pilar Hernández

University of Valencia/IFIC


SM + massive ns

Fogli et al 2012 (after T2K,

Double-CHOOZ, Daya Bay, RENO)

3nmixing:


Standard 3n scenario

The flavour observables:


Goodprospectsfor CP volation

Coloma, Donini, Fernandez-Martinez,PH arXiv:1203.5651


New dofs puzzle

Neutrinos are massive -> there must be new dofs in the SM


New dofs puzzle

Neutrinos are massive -> there must be new dofs in the SM

Weinberg


SM

?

nSM


The good nSM

  • Explanation for the neutrino-charged lepton hierarchy


Thenflavour puzzle I

Why are neutrino masses so light ?


The good nSM

  • Explanation for the neutrino-charged lepton hierarchy

  • Explain the pattern of mixing


Thenflavour puzzle II

CKM

VCKM =

PDG 2007

PMNS

Gonzalez-Garcia, Maltoni

Differences are striking!


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…


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


Outlier I: LSND anomaly

LSND vs KARMEN

Appearance signal with very different

-

Not yet disproved at an acceptable level of confidence…


Pinning down the New physics scale

Hierarchy problem or SUSY ?

eV

keV

MeV

GeV

TeV

meV

Leptogenesis

SUSY GUTs


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


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 !


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


Occam’s razor


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


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


d=6 phenomenology

Long listofflavoured-operators

  • rareleptondecays: m -> e g

  • Z, W decays

  • rhoparameter

  • W mass, …

  • violationsofuniversality, unitarity,…

But…


la -> lbg

MEG

Ifjust neutrino masses:

Ifalsod=6 [email protected]


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


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)


BSM and Neutrino Masses(Up->Down approach)

?


New physics scale

Type I see-saw: interchange a heavysingletfermion

Minkowski; Gell-Mann, RamondSlansky; Yanagida, Glashow…


New physics scale

Type II see-saw: interchange a heavy triplet scalar

Konetschny, Kummer; Cheng, Li; Lazarides, Shafi, Wetterich…


New physics scale

Type III see-saw: interchange a heavy triplet fermion

Foot et al; Ma; Bajc, Senjanovic…


New physics scale

Alsofromloops !

Zee-Babu

Systematicexplorationof 1-loopgenerated Weinberg interaction

Bonnet et al 2012


Effectivesee-sawtheories

Alsod=6operators

Type I

Non-unitarity in

mixing !

Type III

Type II

Gavela, Broncano, Jenkins; Abada, et al


Type I Seesaw

Most general (renormalizable) Lagrangian compatible with SM

gauge symmetries:

Y: 3 xnRMN: nRxnR

mn

ms


Onescalesee-sawmodels

Ye


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


MinimalFlavour type I seesaw model

Gavela, Hambye, Hernandez, PH 09

Only two extra Weyl fermions + SM

Y, Y’ complex vectors, L, m, m’ numbers


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


Complementarityof CLFV and neutrino oscillations

NH

IH

Gavela, Hambye, Hernandez, PH 09


CLFV within reach

Dinh, Ibarra, Molinaro, Petcov 2012


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…


MinimalFlavourSee-sawIII at LHC

Eboli, Gonzalez-Fraile, Gonzalez-Garcia 2011


CMS-PAS-HIG-12-005

Type II seesaw


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 ?


Outlier II: reactor anomaly

old fluxes underestimated by 3%:

Re-calculation of reactor fluxes:

Mueller et al, ArXiv: 1101.2663


Outlier III: Cosmology

Hamann et al, ArXiv: 1006.5276

Sterile species favoured by LSS and CMB

Nucleosynthesis:

Izotov, Thuan


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


Pheno 3+ns mixing models ?

Assumes a general mass matrix for 3+ns neutrinos: what is that model ?

3xns

3x3


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)


Type I see-sawmodels

Light sterile states!

De Gouvea, hep-ph/0501039

De Gouvea, J. Jenkins, Vasudevan hep-ph/0608147


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;


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


3+2 MM vs 3+2 PM vs 3n

Donini, PH, Lopez-Pavon, Maltoni, Schwetz ‘12


Heavy-Light Mixings

e

m

t

Large tau mixings to heavy states


Constraint on

Constraint on


BUT….

Significant improvement over 3n scenario, but large tension appearance/disappearance in m sector remains (MINOS CC high energy)

Tension with cosmology that favours extra lighter states

New info from T2K ND ?


We are still lacking an independent confirmation of LSND at the same level of confidence…

New experimental programme ahead by SBL: Mauri’s Talk


A hierarchy ?

?


Conclusions

  • A espectacular experimental progress in neutrino physics has opened

  • a whole new flavour sector in the SM

  • But neutrino masses require new dofs and most probably a new energy scale

  • No hint of the scale…

Dirac n

SUSY-GUTs

1015GeV

0

TeV

Rich phenomenology: must be

explored systematically !


n’s have the highest score at bringing surprises…

….ask these people


BACKUPS


Flavour Symmetries ?

A lot of work has been devoted to justify the tri-bimaximal mixing features of U:

But data is getting further away from TB…

Incorporating deviations very model dependent…


Or Anarchy ?

Doing just fine…

De Gouvea, Murayama 2012


Dark portals

Schabinger, Wells 05

PattWilczek 06

Only two gauge and Lorentz invariant combinations in SM with

d <4

Bosonic

Fermionic

Any hidden sector singlet under SM gauge group can

couple to the dark portals


MiniBOONE-n

Neutrino run

200 MeV≤ En≤ 3 GeV

-

Low energy excess…but not expected if LSND right


MiniBOONE-n

Anti-Neutrino run

Compatible with LSND !

-


Leptogenesis

Mostinterestingandrobustimplicationwiththesemodels

Works out inTypeI Fukuyita, Yanagida,…

Type II Ma,Sarkar, Hambye

Type III Hambye, Li, Papucci, Notari, Strumia

Recentprogress:

flavouredleptogenesis -> followdynamicsof Le, Lm, Lt

Abada, et al; Nardi, et al

Relaxingboundonlight neutrino mass


Leptogenesisstew

But neutrino massmatrixdoesnotprovidetheexactrecipe!

mn < few eV

L violation

MN,D,S > 10 9GeV

CP violation


Type II with LLFV << LLN

If m=0 -> exact L

LLN = MD2/m LLFV = MD

LFV could be measurablefromd=6 operatorsandfullycorrelatedwith

neutrino oscillations

Spectaculareffects at LHC alsofullycorrelatedwith neutrino oscillations


m-> eg

Chakrabortty, Ghosh, Rodejohann


See-saw II: Pair-productionofchargedtripletscalars

pp-> H++ H-- -> l+l+l-l-

Flavour structure one-to-one to mn !BR(H++-> la+lb+ ) ~ |Mab|2

Keung, Senjanovic;…

Han et al;Garayoa, Schwetz; Kadastik,et al ; Akeroyd, et al; Fileviez et al


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