A. Yu. Smirnov

International Centre for Theoretical Physics, Trieste, Italy

as physics phenomenon Measurements

of neutrino

parameters

Study propertiesof medium

Oscillation

tomography

Study properties ofneutrino sources

Searches for New physicsinteractions

Technology Applications

oscillations as a tool

Accomplish ``standard’’ program of determination of of neutrino parameters

Searches for new physics

Mass hierarchy

non-standardinteractions- short range- long range

1-3 mixing

Deviation of 2-3 mixing from maximal

CP-phase

New neutrino

statesEffects of violation of fundamental symmetriesTest of theory of oscillations

Search for new realizations of the oscillation setup Phenomenological consequences

Manipulating with

oscillation setup

Academic interest?

Theory of oscillations: Quantum mechanics at macroscopic distances

Energy-momentum

conservation

Coherence

Entanglment Collective

effects

Interplay of oscillations

with other non-standard

effects

Identify origins of neutrino mass

Oscillation setup for LBL

Neutrinos from pion, muon, nuclei decays Long life-time, large decay pipes straight lines of storage rings

X

T

detector

piontarget

XD

lp

detector

Coherent emission of neutrino by pion along his trajectory

Separation of the WP can be neglected

long pipe

X

T

detector

piontarget

XD

lp

detector

12

detector

A (x,t) = dxS dtS a (xS, tS) exp[ ipS( x - xS) – iES(t – tS)]

pS = p + p – p

Vprod

ES = E + E – E

a (xS, tS) ~ exp[ – ½ tS]

Manipulating with oscillation picture

- Bust the sources- Cut the production region (change length of the decay pipe)- Time window in detection- Collisions of sources - acting on source by magnetic field

E. Akhmedov,D. HernandezA.S.

X

T

detector

piontarget

XD

lp

detector

Coherent emission of neutrino by pion along his trajectory

Decreasing length of decay pipe

X

T

detector

pion

target

XD

lp

detector

muon detectorWith time window

P = P + [cos L + K] sin22 2(1 + 2)

1 1 – e-lp

K = sin L - e [cos(L - p) - sin (L - p)]-lp

L

lp

L = m2 L/2E p = m2 lp/2E

= m2 L/2E decoherence parameter

x

Equivalence

Coherent -emission- long WP

Incoherent -emission- short WP

x

D. Hernandez, AS

MINOS: ~ 1beam ?

at production

P( )

ldecay ~ l

E ~

Coherence:

D. Henandez, A.S.

MINOS,ND

with decoherence

Confronting different effects

Looking for mismatch of parameters determined from different effects

Phase effect Change of mixing in matter does not depend on oscillationphase

Sun

Modified dependence on parameters

Atmosphericvs. SBL

m = mstandard + msoft(E,n) medium (environment ) dependent (``soft’’) component

medium (environment ) dependent (``soft’’) component

Can msoft dominate?Can msoft dominate?

In general:In general:

m(oscillations) = m(kinematics)

Smallness may indicate that nature of the neutrino mass (or at least what we observe in oscillations) differs from masses of other fermions

Is it of the same nature as the mass of electron or top quark?

?

BOREXINO: absence of a significant Day-Night asymmetry for Be-neutrinos

G. Bellini, et al1104.2150 [hep-x]

Excluded one of such scenarios

- Supernova neutrinos – main effect strong adiabatic conversion - Atmospheric neutrinos; - Theory (flavor symmetries)

G.L Fogli et al.,1106.6028 [hep-ph]

TBM

New reactor fluxes- shift by arrows

QLC

m212

m322

Normal mass hierarchy is preferrable

O(1)

sin213 = ½ sin2C

QLC (GUT + BM mixing) Quark-lepton unification + Horizontal symmetry

Naturalness of mass matrix, two largemixings (absence of fine tuning), normal mass hierarchy

Violation of TBM with certain flavor hierarchy of the breaking parameters

T2K: sin213 = 0.028

A cos2 223 - symmetry violation

Accidental?

Disappointing scenario

High scale seesaw

GUTNegligible unitarity violation

Negligible NSI

Flavor physics at very high scales above GUT?

Difference of quarks and leptons is related to smallness of neutrino mass

The same mechanism which

Explains smallness of neutrino mass

is responsible for large lepton mixing

SUSY-?Hierarchy problem?

Hidden sector at GUT, Planck scales

Seesaw enhancement of mixing

No particular symmetry?

QLC: certain symmetries at High scales bi-maximal mixing;Double seesaw?

ur , ub , uj , dr , db , dj , e

urc, ub

c, ujc, c

drc, db

c, djc,

ec

RH-neutrinoRH-neutrino

S

S

S

S

S SS

S

S

S- Enhance mixing- Produce zero order mixing- Screen Dirac mass hierarchies- Produce randomness (anarchy)- Seesaw symmetries- Sterile- Violation of unitarity

SS

S

S

SS

S

SS

SSSS

SS

S

S

S

S

Hidden sector

Normal mass hierarchyee

e e

eesin2 213 = 0.050

contours of constant oscillation probability in the energy- nadir (or zenith) angle plane

The Earth in neutrino light

sin2 213 = 0.125

Normal mass hierarchy

= 60o

Standardparameterization

= 130o

= 315o

formed bygrids of magic linesand lines of interference phase

formed bygrids of magic linesand lines of interference phase

P() – P P() – P

CP-violationdomains

P

CP-violationdomains

P

P

10

1

100

0.1

E,

GeV

MINOS

T2K

CNGS

NuFac 28000.005

0.03

0.10

T2KK

Degeneracyof parameters

IceCube

LENF

IC Deep Core

NOvA

PINGU-1

e

contours of constant oscillation probability in energy- nadir (or zenith) angle plane

Challenge for theory, phenomenology experiment

(2 – 4) 10-3 eV

0.5 - 2 eV

~ 10 keV

40 - 70 MeV - LSND, MiniBooNE

- Warm Dark matter- Pulsar kick

- Solar neutrinos- Extra radiation in the Universe

- LSND, MiniBooNE- Reactor anomaly- Calibration experiments- Extra radiation

s

1 eV

1 keV

1 MeV

10-3 eV

e

2

1

4

mas

s

m2atm

m2sun

3

m2LSND

s

P ~ 4|Ue4 |2|U4 |2

restricted by short baseline exp. BUGEY, CHOOZ, CDHS, NOMAD

LSND/MiniBooNE: vacuum oscillations

With new reactor data:

m412 = 1.78

eV2Ue4 = 0.15 U4 = 0.23

P ~ 4|Ue4|2 (1 - |Ue4|2)

For reactor and source experiments

- additional radiation in the universe- bound from LSS?

( 0.89 eV2)

mee me me … m m … … m For mSS ~ 1 eV

For mSS ~ 1 eV

Mass matrix

Mass matrix

e

e

meS mS mS

mSS … … …

SS

tanjS = mjS/mSS

mSS >> mab , maS mSS >> mab , maS

~ 0.2 - is not small

large corrections to the active neutrino mass matrix

In general can not be considered as small perturbation!

mij ~ - taniStanjS mSS ~ 0.04 mSS

Active neutrino spectrum is quasi degenerate

meS mS mS have certain symmetry

Effect can be small if

mSS ~ mab mSS ~ mab

J. Barry, W. Rodejohann,He ZhangarXiv: 1105.3911

m = ma + m

produce dominant - block

with small determinant

Original active mass matrix e.g. from see-saw

Original active mass matrix e.g. from see-saw

m can change structure (symmetries) of the original mass matrix completely (not a perturbation)

m can change structure (symmetries) of the original mass matrix completely (not a perturbation)

Induced mass matrix due to mixing with nu sterile

Induced mass matrix due to mixing with nu sterile

Enhance lepton mixing

Generate TBM mixing

UPMNS

Be origin of difference of

VCKMand

In assumption of no-oscillations in ND

|U4|2 < 0.015 (90% CL) 13 = 0

|U4|2 < 0.019 (90% CL) 13 = 11.5o

LSND/MiniBooNE:

|U4|2 > 0.025

m412 < 0.5 eV2

- s mixing

cosmology

BUGEY+MINOS

H Nunokawa O L G PeresR Zukanovich-FunchalPhys. Lett B562 (2003) 279

S Choubey HEP 0712 (2007) 014

- s oscillations with m2 ~ 1 eV2 are enhanced in matter of the Earth in energy range 0.5 – few TeV

IceCube

This distorts the energy spectrum and zenith angle distribution of the atmospheric muon neutrinos

S Razzaque and AYS , 1104.1390, [hep-ph]

Antineutrinos

MSW resonance dip

Neutrinos

Eth = 0.1 TeV

S = N(osc.)/N(no osc.)

For different mixing schemes

Varying |U0|2

sin2 = s24

2 s24

2 + s342

S - mass mixing case

Free normalization and tilt factor

e

2

1

0

mas

s m2atm

m2sun

3

m2dip

s

- additional radiation in the Universe if mixed in 3

- no problem with LSS (bound on neutrino mass)

Very light sterile neutrino

- solar neutrino data

Motivated by

pp 7Be CNO 8B

gap

e- survival probability from solar neutrino data vs LMA-MSW solution

- dip- wiggles

sin22= 10-3 (red), 5 10-3 (blue)

SK-I

SK-III

SNO-LETA

R = 0.2

m2 = 1.5 10-5 eV2

SNO-LETA

Borexino

P. De Holanda, A.S.

S. Abe, at al., [The KamLAND collaboration]1106.0861 [hep-ex]

sin2 2 ~ 10-3

m0 ~ 0.003 eVM2 MPlanck

m0 = M ~ 2 - 3 TeV

mixing h vEW M

~

sin2 2 ~ 10-1 vEW M ~

h = 0.1

IceCube DeepCore

difference

With sterile

MINOS as a modelMiniBooNE

Increase of base-line matter effects but no enhancement for large…

Near detectors…

ND FD

averagedoscillation effect

Non-averagedeffect

1 – 3 km

m412 ~ 1

eV2

No matter enhancement

m432 ~

0.0025eV2

Very small effect

Matter enhancement: Resonance at E= 12 GeV

Non-averagedeffect

-disappearance

A la LSND –e

–s

suppressed, difficult to extract from BGand usual oscillation channels (FD)

distortion of spectrum

CC NSI CC NSI

NC NSImatter NSI

Interesting physics:

e

- Zero distance LFV- Oscillation enhancement of the NSI effect (interference with oscillation linear effect in ) - Modification of matter potential - Effect does not disappear with increase of E

Motivation: - MINOS anomaly- Solar- MiniBooNE

Expectation ?

Ad hoc assumptions

< 10-2 to be further affected by LHCBounds:

Large 1-3 mixing: Discrete symmetries? TBM accidental? QLC? Quark-lepton unification? Possible: GUT + high scale seesaw + fermion singlets (hidden sector) with some symmetries?

Physics of oscillations: various conceptual issues;

coherence at production. In future a possibility to manipulate

with neutrino wave packets

New (still controversial) evidences of new neutrino states = sterile neutrinos.

Tests: with Solar and atmospheric neutrinos IceCube, Deep-Core IC

1-3 mixing, Mass hierarchy, CP (?) with atmospheric neutrinos and DeepCore IC, PINGU-I, INO

1. Experiment: deviations from TBM mixingRGE-effects

2. No simple and convincing model for TBM

- Complicated structure, large number of assumptions

and new parameters

- Follows from certain correlation of unrelated sectors

3. Often: no connection between masses and mixing additional symmetries are introduced

4. Inclusion of quarks: further complication. GUT – additional requirements

Numerology without underlying frameworkInterplay of various independent contributions

Symmetry mass relations can be broken maximally

E Giusarma et al 1102.4774 [astro-ph]

run 1 (blue)

95%68 %

m2 < 0.25 eV2

run 2 (red)

- WMAP- SDSS (red galaxy clustering)- Hubble (prior on H0 )

- Supernova Ia Union Compilation 2 (in add)

+ BBN

Inverse approach:

J R Kristiansen, O Elgaroy 1104.0704 [astro-ph]

wCDM + 2S

1). w < -1

2). Age of the Universe 12.58 +/- 0.26 Gyr

too young?

The oldest globular clusters 13.4 +/- 0.8 +/- 0.6 Gyr

ruling out

CDM

(- 0.7 – 0.8)

(- 0.9 - 0.8)

(- 1. - 0.9)

50 Mt yr

Blue – normalRed – inverted1 error

For different zenith angle bins

O. Mena, I Mocioiu, S. Razzaque, arXiv:0803.3044

IceCubeDeep core

1-3 mixing, Mass hierarchy, CP (?) with atmospheric neutrinos and DeepCore IC, PINGU-I, INO

And by studies of the atmospheric neutrinos by IceCube, DeepCore IC, and in future PINGU open very interesting possibilities to study oscillations of high energy neutrinos: searches for sterile, identify hierarcy and probably measure CP. More studies is needed (may be some upgrate of PINGU)

INO: with large 1-3 mixing a possibility to establish mass hierarchy.

Implications of large 1-3 mixing: weaken the case of symmetry (TBM) More towards usual situation with enhances lepton mixing due to seesaw

Rich phenomenology - propagation - detections

Rich phenomenology - propagation - detections

High energies where usual

mixing is suppressed …High energies where usual

mixing is suppressed …

Checks at LHC, Rare processes with L-violation

Checks at LHC, Rare processes with L-violation

M. Blennow, T. Ohlsson, 0805.2301M. Blennow, T. Ohlsson, 0805.2301

13 = 8o

e ~ - 0.5 sin2

standardstandard

Pee

white: strong transitionwhite: strong transition

Smallness of neutrino mass

High scale, MPl , Mstrings

Violation ofSymmetriesat this high scales

Heavy particle exchange

Heavy particle exchange Light particlesLight particles

New scalars exchange New scalars exchange

SUSY with R-parity breakingSUSY with R-parity breaking

New scalarsNew scalars

Majorons,Accelerons Cosmons…

Majorons,Accelerons Cosmons… With some

cosmologicalmotivations

With some cosmologicalmotivations

Restrictions: see talk S. Hannestadt

Restrictions: see talk S. Hannestadt

Phenomenology: T. OtaPhenomenology: T. Ota

tan

m1/eV

m1/eV

MSSMMSSMSMSM

positivepositive

M. A. Schmidt, A.S. hep-ph/0607232

M. A. Schmidt, A.S. hep-ph/0607232

seesaw-I bi-maximal mixing,seesaw-I bi-maximal mixing, mD ~ mu ml ~ md

K. Babu, R. Mohapatra, Matsuda, B.Bajc, G. Senjanovic, F.Vissani, Goh, Ng ...

Mu = Y10 vu10

+ Y126 vu126

Large 2-3 mixing needs b - unification

``Minimal SO(10)’’:

Fermion masses (Yukawa couplings) due to 10H and 126H

Mass matrices

Md = Y10 vd10

+ Y126 vd126

Ml = Y10 vd10

- 3Y126 vd126M = kY126

Assumption: Seesaw II gives main contribution

M ~ Ml - Md

For second and third generation

tan223 ~

2sin23q

2sin2 23q - (mb - m)/mb

S. Bertolini, et al

productionregion

detectionregion

baseline L

i

Two interaction regionsin contrast to usual scatteringproblem

Externalparticles

Neutrinos: propagator

Finite space and time phenomenon Finite space-timeintegration limits

wave packets for external particles

encode info about

finite production and

detection regions

Formalism should be adjusted to these condition

E. Akhmedov, A.S.

a phenomenon in which neutrino state changes (or quasi periodically) its flavor as it propagates in space-timeIt is induced by monotonous between eigenstates of propagation (mass states in vacuum) which compose a neutrino state

In contrast to e.g. adiabatic conversion which is related to

in process of propagation

Energy-momentum

conservationEntanglment

Coherence

under discussion challenging standard picture of oscillations

K Abe, et al [The T2K Collaboration]1106.2822 [hep-ex] for maximal 2-3 mixing

Background = 1.5+/-0.3 sin213 ~ 0.11

core

mantle

Flavor-to-flavor transitions

Oscillations in multilayer medium

- nadir angle

core-crossingtrajectory

-zenith angle

= 33o

acceleratoratmosphericcosmic neutrinos

Applications:

Neutrinointeractions

generated by L L H H1

S. Weinberg

~ 1014 GeV << MPlNew physics below Planck scale

If R exists: MR ~

H HL

R

~ 2

SUSY ?

Dirac mass

- small Yukawa coupling- additional doublet with small VEV

No other manifestations of new physics

DM?

Correspondence: ur , ub , uj <-> dr , db , dj <-> e

Symmetry: Leptons as 4th color

Unification:Form multiplet of the extendedgauge group, in particular, 16-plet of SO(10)

Pati-Salam

Can it be accidental?

Minimalist approach’’M. Shaposhnikov et al

Unification of - quarks & leptons - couplings

m = - mDT mD

RH neutrino components have large Majorana mass 1

MR

MGUT2

MPl

MGUT

MR ~

in the presence of mixing

MGUT ~ 1016 GeV

Neutrino mass as an evidence

of Grand Unification ?

N l + HLeptogenesis:the CP-violating out of equilibrium decay

lepton asymmetry baryon asymmetry of the Universe

mD ~ mD(q, l)

Contour plots for the probability difference P = Pmax – Pmin

for varying between 0 – 360o

e

Emin ~ 0.57 ER

Emin 0.5 ER

when 13 0

Near Detector

rNC = nNC nNC

0

P rNC

Far Detector:

P

D. Henandez, A.S.1105.5946 [hep-ph]

0.5

1

2

4

8

m422

sin2 224 = 0.1

Neutrinos from pion, muon, nuclei decays

Long life-time, large decay pipe in the case of pions

Long straight lines of storage rings where neutrino fluxes are formed

Large neutrino production regions can be comparable with oscillation length

Coherence at production:

E < m2/2E

Strongly broken TBM? Typical for flavor models of TBM: sin13 ~ sin2C

Quark-lepton complementarity:

No special symmetry in the leptonic sector

sin2 213 ~ 2sin2C

Mixing appears as a result of different ways of the flavor symmetry breaking in neutrino and charged lepton sectors

Gf

Gl

Symmetry is not broken completely; residual symmetries

in the neutrino and charged lepton sectors are different

G

Residual symmetries

M TBM-type

Ml diagonal

In turn, this split originates from different flavor assignments of the RH components of Nc and lc and different higgs multiplets

No exact flavor symmetry

1