A. Yu. Smirnov International Centre for Theoretical Physics, Trieste, Italy Latsis Symposium 2013,...
-
Upload
jarod-rowling -
Category
Documents
-
view
217 -
download
0
Transcript of A. Yu. Smirnov International Centre for Theoretical Physics, Trieste, Italy Latsis Symposium 2013,...
A. Yu. SmirnovInternational Centre for Theoretical Physics, Trieste, Italy
Latsis Symposium 2013 , ``Nature at the Energy Frontiers’’ ETH Zurich, June 3 – 6, 2013
Neutrinos and LHC
Smallness is related to existence of new physics at high energy scales
Mnew ~
(VEW ) 2
mn
GUT scaleLeptogenesis
Studying neutrino mass and mixing
probe of new
physics at these
scales
TeV scale mechanisms of neutrino mass generation ?
Atmospheric neutrinos in Ice Cube E = 4 102TeV
~ 1010 - 1016 GeV s = (1 TeV )2
Cosmic neutrinos ( ?) with
E ~ 103 TeV
Discovery of the 1-3 mixing
All well established/confirmed results are described by
Discovery of
cosmic neutrinos
of high energies ?
Reactor, Galllium
LSND, MiniBooNE
New solar neutrino anomaly
Additional
radiation in
the Universe
Connected ?
1 eV sterile neutrino: not a small perturbation of the 3n picture
- Mass hierarchy
- CP violation
- absolute scale
- nature
(Majorana?)Theory beyondWeinberg operator?
January 2012
August 2012
M.G Aarsten, et al. arXiv:1304.5356 [astro-ph.HE]
E = 1.14 +/- 0.17 PeV
E = 1.04 +/- 0.16 PeV
Atmospheric neutrino background: 0.082 +/- 0.004 (stat) +0.041/–0.057(syst.)p-value 2.9 10-2 (2.8s)``Hint’’ of cosmic neutrinos or Excess at lower energies 0.02 – 0.3 PeV 28 events (7 with muons) are observed ~ ~ 11 expected
New physics with atmospheric neutrinos
Centers of two cascades
MSW-effect
Oscillations
Can be resonantly enhanced in matter
Parametric efects
In wide energy range: from 0.3 MeV to 30 GeVconfirming standard oscillation picture with standard dispersion relations
Daya Bay
MINOS
KAMLAND
15 years after discovery: routinely detect oscillation effects
nm nt
ne
n2
n1
MA
SS n1
n2
n3
n3
MA
SS
Dm223Dm2
32
Dm221
Dm221
Inverted mass hierarchyNormal mass hierarchy
?
Dm232 = 2.4 x 10-3 eV2
Dm221 = 7.5 x 10-5 eV2
Two large mixings
(cyclic permutation)
For antineutrinos spectra are
different (distribution of the nm
and nt - flavors in n1 and n2)
due to possible CP-violation
1-3 mixing
Symmetry: TBM?
sin2 q13
0.0 0.010 0.020 0.030 0.040
RENO, 1s
Fogli et al, 1s
T2K 90%
QLC
Double Chooz, 1s
Daya Bay, 1s
- m t breaking
mass ratioGonzalez-Garcia et al, 1s
sin2 q23
0.30 0.35 0.40 0.45 0.50 0.55 0.60 0.65 0.70
MINOS, 1s
SK (NH), 90%
Fogli et al, 1s
SK (IH), 90%
QLC
Gonzalez-Garcia et al, 1s
symmetry
``Naturalness
’’Absence of
Fine tunning
of mass
matrix
Dm21
2 Dm32
2
O(1)
sin2q13
~ ½sin2qCQuark- Lepton ComplementarityGUT, family symmetry
~ ½cos2 2q23
nm - nt – symmetryviolation
The same 1-3 mixing with completely different implications
q13 + q12 = q23
Mixing
anarchy
> 0.025
Self-complementarity
~ ¼ sin2q12sin2q23Analogy
with quark
mixing
relation
q13 = 21/2( /4p -
q23)
1/3 – |Ue2|2 ~ sin2q13
Large scale structure
of the Universe
S m < 0.23 eV (68 % CL)
SDSS
KATRIN
meeff < 2.2 0.2 eV (90%
CL)
Cosmology (Planck BAO)
Oscillations
m > Dm312 > 0.045 eV
m2 m3
Dm21
2 Dm32
2
~ 0.18>
Direct kinematic measurements (future)
NH
Dm21 m1
~ = 1.6 10-
2
Dm212
2 Dm32
2
IH
The weakest hierarchy Strong degeneracy symmetry
mee = Sk Uek2 mk ei ( )f k
x
p
p
n
n
e
e
n mee
W
W
mee = Ue12 m1 + Ue2
2 m2 eia + Ue32 m3
eib76Ge 76Se + e + e Qee = 2039 keV
5 detectors, 71.7 kg yr
mee = (0.29 – 0.35) eV
Heidelberg-Moscow
EXO-200
mee < (0.14 – 0.38) eV
Xe- Observatory136Xe
m1
Heidelberg-Moscow
GERDA II
CUORE
GERDA I
NEMO
GERDA II
Cuoricino
EXO-200
Upper bounds, boxes – uncertainties of NME
S M Bilenky C Giunti arXiv:1203.5250 [hep-ph]
EXO-200: mee < (0.14 – 0.38) eV
H-M: mee = (0.29 – 0.35) eV
KamLAND-Zen
EXO and Kamland-ZenAlmost exclude H-M (interpretation in terms of light Majorana neutrinos
Phase I in absense of signal for 20 kg year: T1/2 > 1.9 1025 yr (90%
CL)
GERmanium Detector Array
3s range: (0.69 – 4.19) 1025 yr
T1/2 = 1.19 1025 yr
Heidelberg- Moscow:
Can confirm but not exclude completely
Blind analysis, the box should be opened now
Phase II: 37.5 kg y: 0.09 – 0.29 eV
Phase III: 1 ton 0.01 eV
In spite of 1-3 mixing determination…
~ 10-9 – 1019 GeV
from symmetry
and hierarchy
far from real understanding this new physics?
anarchyto
Still at the cross-roads
from eV to Planck
Phenomenology: to a large extend elaborated
Discovery of new physics BSM in some other sectors would have …..
Some interesting developments along different linesFrom minimalistic scenario of nuMSM to sophisticated structures at several new scales
P. F. HarrisonD. H. PerkinsW. G. Scott
Utbm = U23(p/4) U12
- maximal 2-3 mixing- zero 1-3 mixing- no CP-violation
Utbm = 2/3 1/3 0- 1/6 1/3 - 1/2 - 1/6 1/3 1/2
n2 is tri-maximally mixed n3 is bi-maximally mixed
- sin2q12 = 1/3
L. Wolfenstein
Uncertainty related to sign of 2-3 mixing: q23 = /4 p - /4 p Symmetry from mixing matrix
In the first approximation
0.15
0.62
0.78
Sn
Mixing appears as a result of different ways of the flavor symmetry breaking in the neutrino and charged lepton (Yukawa) sectors. This leads to different residual symmetries
Gf
Gl GnResidual symmetriesof the mass matrices
Mn Ml 1n
A4T’S4 T7
?T Sn
Symmetry transformatiosin mass bases
Generic symetries which do not depend on values of masses to get TBM
Z2 x Z2
Zm
Sn Mn S nT =
MnIn this framework bounds on mixing can be obtained without explicit model-building
In flavor basis SiU
( UPMNS Si UPMNS
+ T ) p = I
D. Hernandez, A.S.1204.0445
Explicitly
(SiU T) p = I (SiU T) p = (WiU) p = I
The main relation: connects the mixing matrix and generating elements of the group in the mass basis
Equivalent to
Tr ( UPMNS Si UPMNS + T ) = a Tr (WiU) = a
a = Sj lj
ljp = 1
lj - three eigenvalues of WiU
j = 1,2,3
Transformations should be taken in the basis where CC are diagonal
In flavor basis
Also S. F. Ge, D. A. Dicus, W. W. Repko, PRL 108 (2012) 041801
|Ubi|2 = |Ugi|2 |Uai|2 =
For column of the mixing matrix:
1 – a 4 sin2 (pk/m)
k, m, p integers which determine symmetry group
S4
D. Hernandez, A.S.
d = 1030
ka = 0
a = 0
If symmetry transformations Sn depend on specific mass spectrum, Relations include also masses and Majorana CP phases
D. Hernandez, A Y S. 1304.7738 [hep-ph]
sin2 2q23 = sin d = cos k = m2 /m1 = 1
ur , ub , uj , n dr , db , dj , e
urc, ub
c, ujc,
nc
drc, db
c, djc,
ec
RH-neutrino
S
S
S
S
S SS
S
S
S- Enhance mixing- Produce zero order structure- Randomness (if needed)
SS
S
S
SS
S
SS
SSSS
SS
S
S
S
S
Hidden sector
SO(10) GUT + …
High scale mass seesaw
Explains smallness of neutrino mass and difference of q- and l- mixings
Possibly some Hidden sector at GUT - Planck scales
Flavor symmetries at very high scales, above GUT?
Old does not mean wrong
Tests of the low (TeV) -scale mechanisms of neutrino mass generation
R-parity violation
Low scale Seesaw
Of different types
at LHC
RH neutrinos at LHC
Tests of BSM framework which can lead to the neutrino mass generation
Tests of the physics framework SUSY, extraD …
No good motivations
Search for mediators of seesaw, accompanying particles
Radiative mechanisms
lType-Ii
l l j j
x
q
q l
NWR
bi-leptons with the same-sign
SenjanovicKeung
WR*
q
qbb0n
s (jj l) = mN2
No missing energyPeaks at
s (jj ll) = mW
2
Also opposite sign leptons
nn
P.S Bhupal Dev, et al, 1305.0056 [hep-ph]
Mix with active neutrinos
ns
No weak interactions:- singlets of the SM symmetry group
LightRH-components
of neutrinos
may have Majorana masses maximal mixing?
Sov. Phys. JETP 26 984 (1968)
Pisa, 1913
Dear Dr. Alexei Yu. Smirnov, Please pay attention to our upcoming Special Issue on "Research in Sterility" which will be published in the"Advances in Sexual Medicine" , an open access journal. We cordially invite you to submit your paper …
LSND MiniBooNE
Gallex,GNO
SAGE
G.Mention et al, arXiv: 1101.2755P Huber
Dm412 = 1 - 2
eV2
nm
nt
ne
n2
n1
n4
mas
s
Dm231
Dm221
n3
Dm241
ns
P ~ 4|Ue4 |2|Um4 |2
restricted by short baseline exp. BUGEY, CHOOZ, CDHS, NOMAD
LSND/MiniBooNE: vacuum oscillations
With new reactor data:
Dm412 = 1.78
eV2Ue4 = 0.15 Um4 = 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)
All positive evidences vs null results
Tension between disappearance data and νμ → νe LSND-MiniBooNE signals
J. Kopp , P. A. N. Machado, M. Maltoni, T. Schwetz, 1303.3011 [hep-ph]
cosmology
0PERA
OPERA, Collaboration 1303.3953 [hep-ex]
Controversialsituation
Neff = 3.30 (95 % CL) + 0.54- 0.51
Neff = 3.30 +/- 0.27 (68% CL)
Inconclusive
Effective number of neutrino species
BBN
Neff = 3.68 (68 % CL) + 0.80- 0.70
Y. I. Izotov and T X Thuan Astrophys J 710 (2010) L67
After Planck
Planck +WP+highL+BAO
Neff = 3.62 (95 % CL) + 0.50- 0.48 Planck +WP+highL +
H0
NESSiE
Neutrino Experiment with Spectrometers in Europe, Charged Current (CC) muon neutrino and antineutrino interactions. two magnetic spectrometers located in two sites:"Near" and "Far" from the proton target of the CERN-SPS beam. complemented by an ICARUS-like LAr target For (NC) and electron neutrino CC interactions reconstruction.
arXiv: 1304.7127 [physics.ins-det]
NUCIFER Very short baseline reactor experiment
Source experiments
SCRAAM
OscSNS BooNE
Accelerator SBL experiments MicroBooNE (LArTPC),
Tens kilocurie source 50 kCi 144Ce - 144Pr (3 MeV) or 106Ru - 106 Rh (3.54 MeV)
MiniBooNE + SciBooNE
BOREXINO, KamLAND, SNO+
M. Cribier et al, 1107.2335 [hep-ex]]
SOX 51Cr G Bellini et al 1304.7721
H Nunokawa O L G PeresR Zukanovich-FunchalPhys. Lett B562 (2003) 279
S Choubey JHEP 0712 (2007) 014
nm - ns oscillations with Dm2 ~ 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]
Possible distortion of the zenith angle distribution due to sterile neutrinos
Varying |Ut0|2
< 3% stat. error
no sterile
IC79
Less than 5% puls
A. Gross, 1301.4339 [hep-ex]
CC interactions, muon tracks
A Esmaili, AYS
With 5% uncorrelated systematics
nmnt
ne
n2
n1
n0
mas
s Dm231
Dm221
n3
Dm2dip
ns
- additional radiation in the Universe if mixed in n3
Very light sterile neutrino
- solar neutrino data
Motivated by
no problem with LSS (bound on neutrino mass)
m0 ~ 0.003 eV
can be tested in atmospheric neutrinos with DC IceCube
sin2 2a ~ 10-3
sin2 2b ~ 10-1
DE scale?
M2 MPlanck
M ~ 2 - 3 TeV
pp 7Be CNO 8B
ne - survival probability from solar neutrino data vs LMA-MSW solution
HOMESTAKE low rate
.pep
SNO
SNO+
m0 ~ 0.003 eV
M2 MPlanck
m0 =
M ~ 2 - 3 TeV
P. de Holanda, AYS
L R
NormalMass hierarchy
3- 10 kev - warm dark matter - radiative decays X-rays
Few 100 MeV
- generate light mass of neutrinos- generate via oscillations lepton asymmetry in the Universe- can beproduced in B-decays (BR ~ 10-10 )
split ~ few kev
M. Shaposhnikov et al
Phenomenology of
sterile neutrinos
nBAU
WDM
Everything below EW scale small Yukawa couplings
EW seesaw
Neutrino mass hierarchy
CP-violation
deviation of
2-3 mixing
from maximal Absolute
mass scale
Majorana
nature Searches for bb0n- decay
Checks of existence of sterile neutrinos
Study of geo-neutrinos
Solar neutrinos: DN - asymmetry, CNO, spectral upturn
Detection of high energy cosmic neutrinos
Neutrinos and
cosmology:
connections of
neutrinos to the dark
Universe
Detection of Galactic SN neutrinosrelic SN
neutrinos
Reconstruction of the mass and mixing spectrum
Astrophysics
Majoran
aphases
Earth matter effectEnergy spectrsNOvA
Neutrino beam Fermilab-PINGU(W. Winter)
Sterile neutrinos may help?
NH IHnu antinu
Strong suppression of the ne peak NH ne n3
in neutrino channels NH in antineutrino IH
Shock wave effect
in the antineutrino
channel only NH
in the neutrino channel only IH
If the earth matter effect is observed for antineutrinosNH is established!
Permutation of the electron and non-electron neutrino spectra
Neutrino collectiveeffects
Time rise of the anti-ne burst initial phase IH
more in IH case,spectral splits at high energies IH
P. Serpico et al
Earth matter effects
G Fuller et alB Dasgupta et al
A. Dighe, A. S.
C. Lunardini
G. Fuller, et alR. Tomas et al
The neutrino oscillation probability at baselines of 295 (left), 810 (middle), and 7500 km (right) as a function of the neutrino energy. The red (blue) band corresponds to the normal (inverted) mass hierarchy and the band width is obtained by varying the value of . The probabilities for look similar with the hierarchies interchanged. Note the different scales of the axes.
M. Blennow and A Y Smirnov Advances in High Energy Physics Volume 2013 (2013), Article ID 972485
WC, V = 0.99 MtFid. V = 0.56 Mt 99,000, 20 inch PMTs 20% photocoverage JPARC beam, off-axisBaseline 295 km
Segmented scimtillator detector 14 kTNuMI beamoff-axis (14 mrad) baseline 810 km
CP/MH/astro
CP/MH/osc. parameters
MH/astro
ICAL Iron calorimeterscintillator
MH: 2 - 3 s in half d space
MEMPHYS: CERN - Fréjus tunnel. Two WC tanks 65 m (d) x 103 m (h)
LBNO
LBNE
The LENA (Low-Energy Neutrino Astronomy) 50 kt of liquid scintillator (LSc) tank 32 m x 100 m height.
Oscillation physics with Huge atmospheric neutrino detectors
ANTARES
DeepCore
Oscillations at high energies 10 – 100 GeV in agreement with low energy data
no oscillation effect at E > 100 GeV
Ice Cube
Oscillations 2.7s
M G Aarten et al [IceCube Collaboration]arXiv: 1305.3909
ANTARES
Ice C
ube
Precision IceCube NextGeneration Upgrade
OscillationResearch withCosmics with the Abyss
20 new strings (~60 DOMs each) in 30 MTon DeepCore volume
Few GeV threshold in inner 10 Mton volume
Existing IceCube strings
Existing DeepCore strings
New PINGU strings
PINGU v6Denser array
Energy resolution ~ 3 GeV
125m
75m
26m
6 m vertical
DC: h = 350 m d =250
nm + n m+ h
muon track
cascade
Em qm Eh En = Em + Eh Eh Em q m qn
105 events/year
E. Akhmedov, S. Razzaque, A. Y. S.arXiv: 1205.7071
Stot ~ s n1/2
s q ~ 1/E0.5
sE = 0.2E
s q ~ 0.5/E0.5
Smearing with Gaussian reconstruction functions characterized by (half) widths
sE = A E
n
s q = B (mp / E n)1/2
S tot = [S ij Sij2 ]1/2
Improvements of reconstruction of the neutrino angle leads to substantial increase of significance without degeneracy of parameters
sE , GeV 2.3 7.8
E , GeV 10 – 20 20 – 50
Tyce De Young, March 2013
s q 8.3o 4.3o
3, 14o
with experimental smearing
sE = (0.7 En)1/2 y0 = 20o
y-integrated
bad nu – nubar separation
bad angular resolution
Mathieu Ribordy, A. Y .S., 1303.0758 [hep-ph]
Increases significance by 30 – 70 %
sin2 q32, true = 0.42
sin2 q32, fit = 0.50
Shape does not change the amplitude changes
Large significance at low energies
Difficult with PINGU but can be done with next updateWith E ~ 0.1 GeV
The last mixing angle the 1-3 mixing is measured. Strong impact on phenomenology , theory and future experimental programs.
Critical check of the 0nbb - decay observation claim
Studies of atmospheric neutrinos may allow to establish mass hierarchy , measure oscillation parameters, perform searches for sterile neutrinos, non-standard interactions . The fastest, cheapest, reliable way?
Theory: still at the cross-roads. The same 1-3 mixing from different relations with different implications. TBM, Flavor symmetries…?
Sterile neutrinos: challenge for
everything. Ice Cube can help
IceCube: hint for detection of cosmic neutrinos of high energies or new physics in neutrino interactions?
Race for thre neutrino mass hierarchy and CP has started
New important developments (new phase) in the field can
be related to Multi-megaton mass scale under
ice,underwater detectors with low (~1 GeV) energy
threshold (PINGU, ORCA)
indirect connection
Light activeneutrinos
Mechanism of neutrino mass generation
new particles
Mixing pattern
Flavor symmetries
ensure stability of DM particles
play the role of DM
right handed neutrinos
Z2
New neutrinostates
HDM
Warm DM
Directconnection
of the Universe
Dark
Energy
Neutrinos and gravitino as DMW. Buchmueller
Everything from one
P. F. HarrisonD. H. PerkinsW. G. Scott
Utbm = U23(p/4) U12
- maximal 2-3 mixing- zero 1-3 mixing- no CP-violation
Utbm = 2/3 1/3 0- 1/6 1/3 - 1/2 - 1/6 1/3 1/2
n2 is tri-maximally mixed n3 is bi-maximally mixed
- sin2q12 = 1/3
L. Wolfenstein
Symmetry from mixing matrix
0.15
0.62
0.78
Dominant approach
Form invariance
D. Hernandez, A.S.to be submitted
- bounds on moduli of matrix elements- elements of a given column j determined by
index of S - two relations corresponding to real and imaginary
of a- the column j is completely determined
Tr (WiU) = Tr ( UPMNS Si UPMNS + T )
Sa (2|Uaj|2 – 1) e = a
ifa
|Uej|2 =
aR cos (fe /2) + cos (3fe /2) – aI sin (fe /2) 4 sin (fe m /2) sin (fte /2)
f ab = fa - fb
aR cos (fm /2) + cos (3fm /2) – aI sin ( fm /2)
4 sin (fe m /2) sin (fmt /2) |Umj|2 =
Interesting possibilities
2/31/61/6
For i =1 Trimaximal 1
1/31/31/3
For i = 2 Trimaximal 2
1/41/21/4
T (SiU T) = WiU
Another class of possibilities: with (m – p) permutation
corrections wash out sharp difference of elements of the dominant mt-block and the subdominant e-line
Values of elements gradually decrease from mtt to mee
This can originate from power dependence of elements on large expansion parameter l ~ 0.7 – 0.8 . Another complementarity: l = 1 - qC
Froggatt-Nielsen?
Number of photo-electons
Also excess of events at lower energies:
27 events are observed12 are expected
Atm. Neutrino Background: 0.082 +/- 0.004 (stat) + 0.041 / – 0.057(syst.)
0 mDT 0
mD 0 MDT
0 MD m
mn = mDT MD
-1T m MD-1 mD
Beyond SM: many heavy singlets…string theory
R.N. MohapatraJ. Valle
Three additional singlets S which couple with RH neutrinos
nnc
S
allows to lower the scales of the neutrino mass generation
m << MD
explains intermediate scale for the RH neutrinos
m ~ MPl, M ~ MGU
m - scale of B-L violation
m = 0 massless neutrinos
M ~ MGU2/MPl ~ 10-14 GeV
violation of universality, unitarity
Inverse seesaw
Cascade seesawm >> MD
(2 – 4) 10-3 eV
0.5 - 2 eV
1 - 10 keV
40 - 70 MeV - LSND, MiniBooNE
- Warm Dark matter- Pulsar kick
- Solar neutrinos- Extra radiation in the Universe
- LSND, MiniBooNE- Reactor anomaly- Ga-calibration experiments- Extra radiation
ns
1 eV
1 keV
1 MeV
10-3 eV
M. Smy
No distortion of the energy spectrum at low energies : the upturn is disfavored at (1.1 – 1.9) s level
Increasing tension between Dm2
21 measured by KamLAND and in solar neutrinos 1.3s level This is how new physics may show
up
nm nt
ne
n2
n1
n1
n2
n3
n3
MA
SS
w32wij = Dm2
ij /2E
D31 ~ 2D32
Inverted hierarchyNormal hierarchy
Oscillations
Mass states can be marked by ne - admixtures
w31
Cosmolog
y
w31
w32
w31 > w32 w31 < w32
makes the e-flavor heavier changes two spectra differently
Fourier analysis
w
S. Petcov M. Piai
Matter effect
bb-decay
J. Kopp , P. A. N. Machado, M. Maltoni, T. Schwetz, 1303.3011 [hep-ph]