Beyond Standard Model and Neutrino Physics Eduardo Peinado - - PowerPoint PPT Presentation

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Beyond Standard Model and Neutrino Physics Eduardo Peinado - - PowerPoint PPT Presentation

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Beyond Standard Model and Neutrino Physics Eduardo Peinado Instituto de Fsica de la UNAM Reunion Anual de la Divisin de Partculas y Campos DPyC SMF 20-22 de Mayo de 2015 BSM Limits on some scenarios by LCH The SM is complete LHC The

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Beyond Standard Model and Neutrino Physics

Eduardo Peinado

Instituto de Física de la UNAM

Reunion Anual de la División de Partículas y Campos DPyC SMF 20-22 de Mayo de 2015

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Limits on some scenarios by LCH

BSM

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The SM is complete LHC

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The SM is complete LHC

Terra cognita and terra incognita

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The SM is complete LHC

Terra cognita and terra incognita

Standard Model & Physics BSM

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Infinite possibilities

  • H. Murayama
  • Many of these extensions

were proposed to address some unsolved questions

  • f the SM: hierarchy

problem, generation and flavour problem

  • Others simply to explain

some deviations of the SM, top forward backward asymmetry, μ→eγ, h→γγ, non universal lepton decays, DM, etc…

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BSM searches

Nothing yet!!! Only limits!!!

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Outline

Introduction

The SM

Neutrino physics

SeeSaw Mechanism

Extensions of the SM Conclusions

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SLIDE 9

The SM

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The SM

➢

The theory describes the fundamental interactions among particles

➢

Based on principle of gauge symmetry

➢

The Higgs Mechanism

1979 1995 1974

1968

1923 1977 1947 1968 1956 1962 2000 1983 1983 1976 1937 1897 HIGGS

The Higgs mechanism for particle masses

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the theory is complete… but what about neutrino physics? cosmology?

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Evidence of Physics BSM

LHC put constraints only in PBSM Neutrino masses * (In the SM L is not violated) Cosmology: Dark Matter, Baryon Asymmetry, Dark Energy … Some theoretical aspects like hierarchy problem something else? LHC? rare decays …

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Neutrinos

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Neutrinos

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Neutrinos

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Neutrino short story

In 1930, Wolfgang Pauli postulated a new particle to explain the apparent non-conservation of energy in radioactive decays. But the theoretical particle he described had properties that made it so elusive that even Pauli wondered whether anyone would ever see it

A revolutions starts that is not finished yet

By 1934, Enrico Fermi had developed a theory of beta decay to include the neutrino, presumed to be massless as well as chargeless.

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Deficit of the solar neutrino flux

Solar neutrino problem

The pioneer experiment of Ray Davis were puzzled by the discrepancy between solar neutrino measurements and the expectations based upon the Standard Solar Model flux calculations

Eric’s talk

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Deficit of the solar neutrino flux

Solar neutrino problem

The pioneer experiment of Ray Davis were puzzled by the discrepancy between solar neutrino measurements and the expectations based upon the Standard Solar Model flux calculations

Eric’s talk

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Deficit of the solar neutrino flux

Solar neutrino problem

The pioneer experiment of Ray Davis were puzzled by the discrepancy between solar neutrino measurements and the expectations based upon the Standard Solar Model flux calculations The flux measured by SNO was consistent with the model

Eric’s talk

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Deficit of the solar neutrino flux

Solar neutrino problem

The pioneer experiment of Ray Davis were puzzled by the discrepancy between solar neutrino measurements and the expectations based upon the Standard Solar Model flux calculations The flux measured by SNO was consistent with the model

Eric’s talk

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Deficit of the solar neutrino flux

Solar neutrino problem

The pioneer experiment of Ray Davis were puzzled by the discrepancy between solar neutrino measurements and the expectations based upon the Standard Solar Model flux calculations The flux measured by SNO was consistent with the model neutrinos change flavour from the sun to the earth

Eric’s talk

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Neutrino Oscillation

Neutrino physics

Bruno Pontecorvo 1957

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Neutrinos

50,000 tons of ultra- pure water.

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how can we give mass to the neutrinos?

Neutrino masses

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how can we give mass to the neutrinos?

Neutrino masses

Neutrinos are neutral particles

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how can we give mass to the neutrinos?

Neutrino masses

Neutrinos are neutral particles If we add a Right-Handed neutrino (singlet of SM) then we have the Yukawa coupling with the Higgs (like quarks and leptons)

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how can we give mass to the neutrinos?

Neutrino masses

Neutrinos are neutral particles

↵i ¯ L↵✏H?Ni

If we add a Right-Handed neutrino (singlet of SM) then we have the Yukawa coupling with the Higgs (like quarks and leptons)

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how can we give mass to the neutrinos?

Neutrino masses

Neutrinos are neutral particles

↵i ¯ L↵✏H?Ni

But there is no symmetry that forbids also this term If we add a Right-Handed neutrino (singlet of SM) then we have the Yukawa coupling with the Higgs (like quarks and leptons)

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how can we give mass to the neutrinos?

Neutrino masses

Neutrinos are neutral particles

Mi ¯ NiNi ↵i ¯ L↵✏H?Ni

But there is no symmetry that forbids also this term If we add a Right-Handed neutrino (singlet of SM) then we have the Yukawa coupling with the Higgs (like quarks and leptons)

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how can we give mass to the neutrinos?

Neutrino masses

Neutrinos are neutral particles

Mi ¯ NiNi ↵i ¯ L↵✏H?Ni

But there is no symmetry that forbids also this term If we add a Right-Handed neutrino (singlet of SM) then we have the Yukawa coupling with the Higgs (like quarks and leptons)

Violates lepton number

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how can we give mass to the neutrinos?

Neutrino masses

Neutrinos are neutral particles

Mi ¯ NiNi ↵i ¯ L↵✏H?Ni

But there is no symmetry that forbids also this term If we add a Right-Handed neutrino (singlet of SM) then we have the Yukawa coupling with the Higgs (like quarks and leptons)

Violates lepton number

Vs.

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Can be either

If Dirac

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Can be either

If Dirac

If we impose Lepton number then the neutrinos are Dirac particles just like quarks and charged leptons many orders of magnitude

mν << me << mt

The Yukawa couplings are very different

Yνe : Ye : Yt

< 10−11 : 10−6 : 1

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If we allow L to be violated?

Majorana Neutrinos

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If we allow L to be violated?

Majorana Neutrinos

The simplest effective source of Majorana neutrino masses dim 5 Weinberg

  • perator
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If we allow L to be violated?

Majorana Neutrinos

The simplest effective source of Majorana neutrino masses dim 5 Weinberg

  • perator

Weinberg, S. (1980)

L = LSM + 1 ΛL5 L5 = LLΦΦ ∆L = 2

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If we allow L to be violated?

Majorana Neutrinos

The simplest effective source of Majorana neutrino masses dim 5 Weinberg

  • perator

Weinberg, S. (1980)

L = LSM + 1 ΛL5 L5 = LLΦΦ ∆L = 2

Implications?

0νββ

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Black Box Theorem

If the neutrinoless double beta decay is observed that will imply a Majorana nature of the neutrinos

. Schechter, J. and Valle, J.W.F. (1982) 


Vs.

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Black Box Theorem

If the neutrinoless double beta decay is observed that will imply a Majorana nature of the neutrinos

. Schechter, J. and Valle, J.W.F. (1982) 


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seesaw

Opening the box (UV completion)

We have several possibilities SU(2) doublets L

2 ⊗ 2 = 1 + 3

type I seesaw

2 ⊗ 2 ⊗ 1 LHN

type II seesaw

2 ⊗ 3 ⊗ 2 L∆L

type III seesaw

2 ⊗ 3 ⊗ 2 LHΣ

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SLIDE 41

seesaw

Opening the box (UV completion)

We have several possibilities SU(2) doublets L

2 ⊗ 2 = 1 + 3

type I seesaw

2 ⊗ 2 ⊗ 1 LHN

type II seesaw

2 ⊗ 3 ⊗ 2 L∆L

type III seesaw

2 ⊗ 3 ⊗ 2 LHΣ

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seesaw

Opening the box (UV completion)

We have several possibilities SU(2) doublets L

2 ⊗ 2 = 1 + 3

type I seesaw

2 ⊗ 2 ⊗ 1 LHN

type II seesaw

2 ⊗ 3 ⊗ 2 L∆L

type III seesaw

2 ⊗ 3 ⊗ 2 LHΣ

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Linear see-saw

More on see-saw

New features emerge when the seesaw is realized with non-minimal lepton content (Isosinglets) SU(2) singlets: (νi

c,Si) 


transforming as 


field L νi +1 N −1 Si +1

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Linear see-saw

More on see-saw

New features emerge when the seesaw is realized with non-minimal lepton content (Isosinglets) SU(2) singlets: (νi

c,Si) 


transforming as 


field L νi +1 N −1 Si +1

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Linear see-saw

More on see-saw

New features emerge when the seesaw is realized with non-minimal lepton content (Isosinglets) SU(2) singlets: (νi

c,Si) 


transforming as 


field L νi +1 N −1 Si +1

violates L in 2 units smallness of neutrino mass is related to the smallness of the parameter mu “natural” in the sense of ’t Hooft

t’Hooft, G. (1982)

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SLIDE 46

Linear see-saw

More on see-saw

New features emerge when the seesaw is realized with non-minimal lepton content (Isosinglets) SU(2) singlets: (νi

c,Si) 


transforming as 


field L νi +1 N −1 Si +1

violates L in 2 units smallness of neutrino mass is related to the smallness of the parameter mu “natural” in the sense of ’t Hooft

t’Hooft, G. (1982)

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Neutrino oscillations 2 flavors

What do we know?

3 mixing angles and 2 squared mass differences weak eigenstates mass eigenstates weak eigenstates mass eigenstates

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What do we know?

Nature of neutrinos Absolute mass scale Mass ordering CP phases Precision in mixing angles

Neutrino mass scale:

Mainz current limit Σ mν < 2 eV Katrin future sensitivity ~ 0.2 eV PLANK+BAO Σ mν <0.23 eV

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What do we know?

Nature of neutrinos Absolute mass scale Mass ordering CP phases Precision in mixing angles

Neutrino mass scale:

Mainz current limit Σ mν < 2 eV Katrin future sensitivity ~ 0.2 eV PLANK+BAO Σ mν <0.23 eV

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Tri-BiMaximal Mixing

Oscillation parameters

Forero, Tortola and Valle, arXiv:1205.4018v2 [hep-ph]

CP mesurable?? Daya Bay: ~ 0.0235

Harriso, Perkin, Scott

bi-maximal tri-maximal

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Tri-BiMaximal Mixing

Oscillation parameters

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Tri-BiMaximal Mixing

Oscillation parameters

Schwetz et al Gonzalez et al Fogli et al Forero et al 2012 Gonzalez-Garcia et al 2012 Fogli et al 2012

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Tri-BiMaximal Mixing

Oscillation parameters

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Tri-BiMaximal Mixing

Oscillation parameters

Forero et al 2012 Gonzalez-Garcia et al 2012 Fogli et al 2012 Forero et al 2012 Gonzalez et al 2010 Fogli et al 2012 Forero et al 2012 Gonzalez-Garcia et al 2012 Fogli et al 2012

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Tri-BiMaximal Mixing

Oscillation parameters

Forero et al 2012 Gonzalez-Garcia et al 2012 Fogli et al 2012 Forero et al 2012 Gonzalez et al 2010 Fogli et al 2012 Forero et al 2012 Gonzalez-Garcia et al 2012 Fogli et al 2012

Tri-Bimaximal and all the models

Predicting zero reactor neutrino RULED OUT!!! THANKS DAYA BAY, T2K ...

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If Majorana

Neutrinoless double beta decay

In the case of 3 active Majorana neutrinos See Eric’s talk IH NH Can also be zero

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If Majorana

Neutrinoless double beta decay

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If Majorana

Neutrinoless double beta decay

1 Dirac + 2 Majorana

Meroni and Peinado (2015)

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Neutrinoless double beta decay

Meroni and Peinado (2015)

2 Dirac + 1 Majorana

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Messing with sterile

More exotic

Meroni and Peinado (2015)

+PseudoDirac See Catalina’s talk

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If type I see-saw

Light Neutrino Masses through see saw

Minkowski,Yanagida, Mohapatra, Senjanovic Sechter, Valle …

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Baryon asymmetry and neutrino mass

The universe consists only on matter

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Baryon asymmetry and neutrino mass

The universe consists only on matter

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Baryon asymmetry and neutrino mass

The universe consists only on matter

B-L

sphalerons violates B and L preserves B-L 't Hooft

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Leptogenesis

If complex Yukawa couplings CP violation

Fong, Gonzalez-Garcia, Nardi, Peinado (2013) Aristizabal-Sierra,Fong, Nardi, Peinado (2014)

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Leptogenesis

If complex Yukawa couplings CP violation

Fong, Gonzalez-Garcia, Nardi, Peinado (2013) Aristizabal-Sierra,Fong, Nardi, Peinado (2014)

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Dark Matter

Zwicky 1933 See one of Eric’s Talks

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Not only in the clusters of galaxies

DM evidence

1969 Vera Rubin Velocidad de las estrellas en la galaxia andromeda Vera Rubin 70's

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Gravitational lensing

DM evidence

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Rotational curves Clusters of galaxies CMB anisotropies BBN ...

See one of Eric’s Talks

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Inventary of matter in the universe

Gas

DM

baryonic matter Non baryonic matter no Stars Stellar gas Gas

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What do we “know” about DM?

Many indirect evidences of DM Constrain the properties of DM Only gravitational up to now

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What do we “know” about DM?

Long lived (Stable) DM cosmological abundance extracted from observations DM is cold ( or warm ) Electrically neutral DM-DM and DM-SM interactions constrained by

  • bservations
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DM puzzle

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DM puzzle

Higgs Portal Direct detection

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Inert scalar DM

One simple Idea for DM

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Inert scalar DM

One simple Idea for DM

H H DM H DM H H DM H DM DM DM DM DM H DM DM

Higgs portal

EWSB

SM + scalar Z2 + -

Deshpande and Ma (1978)

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Neutrino masses in the Inert DM?

L H N η

Z2 + - Z2

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Neutrino masses in the Inert DM?

L H N η

Z2 + - Z2

N

  • T

y p e I S e e s a w

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Neutrino masses in the inert DM

“scotogenic”

  • E. Ma (2006)
  • A. Zee (1980)

Radiative see-saw

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Direct Detection

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Direct Detection

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Flavor Symmetries (Horizontal)

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An example: A4

Ma and Rajasekaran 2001 Babu, Ma, Valle 2003 Altarelli, Feruglio 2005 ...

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A4 and TBM

A4 completely broken

Altarelli Feruglio (2005)

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We have symmetries (stability)?

Z3 in the charged sector Z2 in the neutrino sector

TBM

Hirsch, Morisi, Peinado and Valle

  • Phys. Rev. D 82, 116003 (2010)
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We have symmetries (stability)?

Z3 in the charged sector Z2 in the neutrino sector

TBM

x

stabilize the DM

x

Hirsch, Morisi, Peinado and Valle

  • Phys. Rev. D 82, 116003 (2010)
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We have symmetries (stability)?

Z2 in the charged sector Z2 in the neutrino sector

stabilize the DM

1, 1', 1'' 3

Hirch, Morisi, Peinado and Valle

  • Phys. Rev. D 82, 116003 (2010)
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The simplest model

SM + 3 Higgs SU(2) doublets , 4 right handed neutrinos Charged leptons diagonal

Hirsch, Morisi, Peinado and Valle

  • Phys. Rev. D 82, 116003 (2010)
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The simplest model

SM + 3 Higgs SU(2) doublets , 4 right handed neutrinos

Hirsch, Morisi, Peinado and Valle

  • Phys. Rev. D 82, 116003 (2010)

SM + 3 Higgs SU(2) doublets , 4 right handed neutrinos

Hirsch, Morisi, Peinado and Valle

  • Phys. Rev. D 82, 116003 (2010)
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Neutrino masses in the model

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reactor mixing angle?

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Susy and Proton decay

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Susy and proton decay

Hinchliffe, Kaeding (1993)

  • F. Vissani, (1995).

…

Proton decay

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R-Parity

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Breaking R-parity and neutrino masses

Hall and Suzuki (1984) Mukhopadhyaya, Roy,Vissani (1998)

R-parity breaking gives a contribution to Majorana neutrino mass

Hirsch, Diaz, Porod, Romao, Valle (2000)

Bi-linear R-parity breaking can generate one neutrino mass,

  • ther two by radiative corrections

This case is similar to 1 RH neutrino, rank 1 matrix

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Conclusions

We have evidence of “physics beyond the SM” It is interesting to find scenarios where some of them have a common explanation neutrino physics is a nice “portal to PBSM” DM stability and neutrino physics can be related Neutrino and BAU also related why not neutrinos - DM - BAU

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Conclusions I

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Thank you very much for your attention

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Just in case!!!

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The alignment

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Z2 residual symmetry

Z2 even Z2 odd

Dark Matter Stability

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Relevant Diagrams

Boucenna, Hirsch, Morisi, Peinado, Taoso and Valle JHEP 1105 (2011) 037

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Direct detection

LUX

LUX collaboration arXiv:1310.8214

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Baryon asymmetry

The universe consists only on matter

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Sakharov conditions

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Sakharov conditions

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Sakharov conditions Sakharov conditions

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Sakharov conditions

C:

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Sakharov conditions

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BG in the SM

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Leptogenesis

The simplest way to neutrino masses: Type I see-saw

Minkowski(1977),Yanagida(1979), Gell-Mann et al. (1979), Glashow (1980), Mohapatra and Senjanovic (1981, Schechter and Valle (1980)

We get for free: baryogenesis through leptogenesis [Fukugita and Yanagida (1986)] Conventional Type-I leptogenesis requires

[Davidson and Ibarra (2002)]

Resonant leptogenesis

[Pilaftsis (1997)]

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Leptogenesis

B-L conserved Klinkhamer and Manton

V(υT) υT T <T

EW

T > T

EW

φ

V(φ, T)

Quantum tunneling and Thermal fluctuation EW Vacuum (φmin=v)

T=Tcrit≈TEW

First order phase transition

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Possible models

Type I see-saw

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Possible models

Type I see-saw New scalar that couple to RH neutrino and SM fermions

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Possible models

Type I see-saw New scalar that couple to RH neutrino and SM fermions

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SLIDE 122

Possible models

Type I see-saw New scalar that couple to RH neutrino and SM fermions

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SLIDE 123

Possible models

Type I see-saw New scalar that couple to RH neutrino and SM fermions To match the gauge qn of

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Possible models

Type I see-saw New scalar that couple to RH neutrino and SM fermions ARE NOT SUPERPARTNERS !!!!!!!

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How does it works?