introduction to particle physics: standard model and...
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http://astroparticles.es/
José W F Valle
CINVESTAV 2014
Introduction to particle physics: Standard Model and beyond
Lecture III
Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
confirmed
Where do neutrinos come from?336 / cm3: bilions of Cosmic neutrinos Cross us every second
Necessaryto reviseStandardmodel
confirmed
Valid up to energies ~ 100 GeV, it is the most precise theory of particle interactions we have
At its core are the gauge principle and the Higgs mechanism
The Standard Model
1979199519741968
1923197719471968
1956 1962 2000 1983
1983197619371897
H
Valid up to energies ~ 100 GeV, it is the most precise theory of particle interactions we have
At its core are the gauge principle and the Higgs mechanism
The Standard Model
1979199519741968
1923197719471968
1956 1962 2000 1983
1983197619371897
H
The SM would be completewere it not forneutrinos & cosmology
Valid up to energies ~ 100 GeV, it is the most precise theory of particle interactions we have
At its core are the gauge principle and the Higgs mechanism
The Standard Model
1979199519741968
1923197719471968
1956 1962 2000 1983
1983197619371897
H
The SM would be completewere it not forneutrinos & cosmology
no neutrino massesno dark matterno baryon asymmetryno inflation
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Neutrino oscillations
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Neutrino oscillations
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Neutrino oscillations
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Solarneutrinos
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Survival probability
Solarneutrinos
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Survival probability
DetectionCross section
Solarneutrinos
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Survival probability
DetectionCross section
Solarneutrinos
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Schechter & JV PRD22 (1980) 2227 & PDG
LEPTONIC CKM-MATRIXLEPTONIC CKM-MATRIX
Rodejohann, JV Phys.Rev. D84 (2011) 073011
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Schechter & JV PRD22 (1980) 2227 & PDG
LEPTONIC CKM-MATRIXLEPTONIC CKM-MATRIX
use this approx. in oscillation analyses
Rodejohann, JV Phys.Rev. D84 (2011) 073011
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Schechter & JV PRD22 (1980) 2227 & PDG
LEPTONIC CKM-MATRIXLEPTONIC CKM-MATRIX
use this approx. in oscillation analyses
Rodejohann, JV Phys.Rev. D84 (2011) 073011
DayaBay,RENO,...
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NEUTRINOS IN THE PRECISION ERATHE ERA OF CPV STARTS
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ORIGIN OF NEUTRINO MASS AND SEESAW
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SCALE
MECHANISM
FLAVOR STRUCTURE
ORIGIN OF NEUTRINO MASS AND SEESAW
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SCALE
MECHANISM
FLAVOR STRUCTURE
ORIGIN OF NEUTRINO MASS AND SEESAW
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SCALE
MECHANISM
Minkowski 77 Gellman Ramond Slansky 80 Glashow, Yanagida 79 Mohapatra Senjanovic 80 Lazarides Shafi Weterrich 81 Schechter-Valle, 80 & 82
FLAVOR STRUCTURE
fermion exchange
TYPE I
ORIGIN OF NEUTRINO MASS AND SEESAW
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SCALE
MECHANISM
Schechter-Valle 80/82 Minkowski 77 Gellman Ramond Slansky 80 Glashow, Yanagida 79 Mohapatra Senjanovic 80 Lazarides Shafi Weterrich 81 Schechter-Valle, 80 & 82
FLAVOR STRUCTURE
fermion exchange
TYPE I Scalar-exchange
TYPE II
ORIGIN OF NEUTRINO MASS AND SEESAW
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SCALE
MECHANISM
Schechter-Valle 80/82 Minkowski 77 Gellman Ramond Slansky 80 Glashow, Yanagida 79 Mohapatra Senjanovic 80 Lazarides Shafi Weterrich 81 Schechter-Valle, 80 & 82
FLAVOR STRUCTURE
fermion exchange
TYPE I Scalar-exchange
TYPE II
ORIGIN OF NEUTRINO MASS AND SEESAW
Number & properties of messengers
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SCALE
MECHANISM
Schechter-Valle 80/82 Minkowski 77 Gellman Ramond Slansky 80 Glashow, Yanagida 79 Mohapatra Senjanovic 80 Lazarides Shafi Weterrich 81 Schechter-Valle, 80 & 82
FLAVOR STRUCTURE
LOW-SCALE SEESAW Mohapatra-Valle 86Akhmedov et al PRD53 (1996) 2752 Malinsky et al PRL95(2005)161801 Bazzocchi et al, PRD81 (2010) 051701
fermion exchange
TYPE I Scalar-exchange
TYPE II
ORIGIN OF NEUTRINO MASS AND SEESAW
Number & properties of messengers
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Radiative neutrino mass in 331 scheme
Singer, Valle, Schechter, Phys.Rev. D22 (1980) 738
Boucenna, Morisi, JV Phys.Rev. D90 (2014) 013005
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Radiative neutrino mass in 331 scheme # generations = # colours
Add 3 gauge singlets ...
Singer, Valle, Schechter, Phys.Rev. D22 (1980) 738
Boucenna, Morisi, JV Phys.Rev. D90 (2014) 013005
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Radiative neutrino mass in 331 scheme # generations = # colours
Add 3 gauge singlets ...
Singer, Valle, Schechter, Phys.Rev. D22 (1980) 738
Boucenna, Morisi, JV Phys.Rev. D90 (2014) 013005
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Radiative neutrino mass in 331 scheme # generations = # colours
Add 3 gauge singlets ...
arXiv:1404.3751more on the low-scale approach to neutrino masses ...
Singer, Valle, Schechter, Phys.Rev. D22 (1980) 738
Boucenna, Morisi, JV Phys.Rev. D90 (2014) 013005
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Order in the chaos?
FLAVOR GUT
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Order in the chaos?
FLAVOR GUT
What makes the gauge couplings unify? - A GUT (p decay) - SUSY (LHCII) - NEUTRINO PHYSICS
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Order in the chaos?
FLAVOR GUT
What makes the gauge couplings unify? - A GUT (p decay) - SUSY (LHCII) - NEUTRINO PHYSICS
Boucenna, Fonseca, Gonzalez-Canales, JV arXiv:1411.0566
The physics responsible for gauge coupling unification may also be responsible for small neutrino masses
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Order in the chaos?
FLAVOR GUT
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Morisi et al Phys.Rev. D88 (2013) 036001
Order in the chaos?
FLAVOR GUT
King et al Phys. Lett. B 724 (2013) 68-72
Bonilla et al arXiv:1411.4883
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CHARGED LEPTONS
Sectors are separatedSectors are separatedby an extra Abelian Znby an extra Abelian Zn
THE FLAVORPROBLEM
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CHARGED LEPTONS
Sectors are separatedSectors are separatedby an extra Abelian Znby an extra Abelian Zn
Babu et al PLB552 (2003) 207Hirsch et al PRD69 (2004) 093006
A4
THE FLAVORPROBLEM
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CHARGED LEPTONS
Sectors are separatedSectors are separatedby an extra Abelian Znby an extra Abelian Zn
Babu et al PLB552 (2003) 207Hirsch et al PRD69 (2004) 093006
A4
THE FLAVORPROBLEM
Altarelli, Feruglio 2005
Tri-BiMaximal ansatz Harrison, Perkins, Scott 2000
(CP assummed)
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Problems
Show that in vacuo
Derive
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