non-accelerator neutrino experimentshep.tsinghua.edu.cn/talks/chenshaomin/chen_shaomin.pdf ·...
TRANSCRIPT
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Non-Accelerator Neutrino Experiments
Shaomin Chen
Tsinghua University
2009.11.17
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Outline
Neutrinos in the Standard Model
Neutrino Mixing and Oscillation
Non-Accelerator Neutrino Sources
Underground Neutrino Experiments
Search for Non-Zero 13
Future Prospects
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Neutrinos in the Standard Model
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Neutrinos in Standard ModelNeutrino interactions thru the weak charged current (CC) by exchanging a W boson
and thru the weak neutral current (NC) by exchanging a Z 0 boson
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Dirac Equation
For spin -1/2 particles, the relativistic Dirac equation
i m 0
( ), ( )L RP P 5 5
1 11 1
2 2
By defining two projection operators
Gives two chirality eignspinors,L L R RP P
Dirac equation can thus be expressed as
,i i
R L L Ri ii i m i i m
x x x x
0 00 0
Both equations decouple in the case of zero mass (m=0).
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Helicity & Chirality When m=0
For massless spin -1/2 particle (m=0)
,i i
L L R Ri ii i i i
x x x x
0 0
Identical to the Schrödinger equation in p space
, ,( )L R L RE p , i
ii i E i p
x t x
0
Since the definition of helicity is
| | | |
pH
p
particles particles
antiparticles antiparticlesL RH H
1 1
1 1
Chirality and helicity are identical in this case.
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Case for a Particle with Mass
For massive spin -1/2 particle (m0), since
v cLorentz boost to a new reference frame with a velocity v0
, //v v c v v 0 0
In this new frame
(due to Lorentz boost) (given by natu,| | | | | | | |
re)p p
p p
leading to a sign flip in helicity and chirality eignspinors
L R
no longer describe particles with fixed helicity and
helicity is no longer a good conserved quantum number.
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Neutrinos and Anti-neutrinos
Neutrinos (Left-handed)
Anti-neutrinos (Right-handed) | | | |
1
1
H
p
p
spin spin
momentum momentum
Neutrino(left-handed)
Anti-neutrino(right-handed)
If neutrinos are massless, then helicity is fixed
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Neutrinos Are Left-Handed
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Neutrino Mass In SM
• CPT theorem in quantum field theory
– C: interchange particles & anti-particles
– P: parity
– T: time-reversal
Standard Model: ,R
L
m R LL m
Charged lepton mass term
Analogously, neutrino mass term
m R LL m
R
R
0
0
m
m
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The Solar Neutrino Problem
Standard Solar Model (SSM):
John Bahcall
Experiments (before 2001):
? ? ?Many suspicions on SSM and experiments
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Atmospheric Neutrino Ratio
PDG1998
1998--
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Discovery of Neutrino Oscillation PRL81, 1562 (1998)Evidence for Oscillation of Atmospheric Neutrinos
PRL90, 021802 (2003)First Results from KamLAND: Evidence for Reactor Antineutrino Disappearance
PRL87, 071301 (2001)Measurement of the Rate of e +dp+p+e- Interactions Produced by 8B Solar Neutrinos at the Sudbury Neutrino Observatory
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Neutrino Mass, Mixing And Oscillation
“…I did not believe in neutrino oscillations, even after Davis’painstaking work and Bahcall’s careful analysis: The oscillationswere, I believed, uncalled for. Now, after the beautiful experimentswhich we shall hear about in the next few days, I have to surrenderand accept neutrino oscillations as reality,…” ---C.N. Yang , 2002,opening remarks on “Neutrinos and Implications for PhysicsBeyond the Standard Model”
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Stand Model Extension
L ( )
c
L
( )c
R
R
Majorana
Majorana
Dirac
Le
Re
Le
Re
0
0
me
L ( )
c
L
( )c
R
R
Dm
Lm
Rm
Massive neutrinos indicates new physics beyond SM.
Minimum extension of SM is to allow R’s (Dirac masses) or Lepton number violation (Majorana masses) or both.
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Neutrino Mixinge
L L Le
1 2 3 1
1 2 3 2
1 2 3 3
e e e eU U U
U U U
U U U
cos sin cos sin
sin cos cos sin
sin cos sin cos
1
2
12 12 13 13
12 12 23 23
13 13 23 23
0 0 1 0 0 0 0
0 0 1 0 0 0 0
0 0 1 0 0 0 0 1
ii
i
i
e e
e
e
Pontecorvo
Maki
Nakagawa
Sakata
Standard Model for leptons
Solar Reactor Atmospheric
Dirac phase ,
Majorana phases 1, 2
Extension
This extension introduces 3 masses + 3 angles + 1(3) phase(s) = 7(9) new parameters for SM
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Neutrino Flavor Change In Vacuum
W W
Source Target
l
l
Amp
W W
Source Target
l
l
i
Amp
*
iU i
Ui
2exp[ ]
i
Lim
E
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Neutrino Oscillation
Oscillation probability
Since one mass splitting is observed to be much bigger than the others, we can simply have
Appearance:
Disappearance:
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Two-Flavor Neutrino Oscillation
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Non-Accelerator Neutrino Sources
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Non-Accelerator Neutrino SourcesSergio Pastor, LowNu 2009
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Atmospheric Neutrinos
ee
(
)
)
(
e e
2
ee
Primary cosmic protons strikes atmosphere, producing pions , naively
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Solar Neutrinos
The generated solar neutrinos are all 's and,
there is no at all according to SSM.
e
e
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Supernova Neutrinos
T.Totani, K.Sato,
H.E.Dalhed and
J.R.Wilson,
ApJ.496,216(1998)
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Reactor NeutrinosNeutrinos from beta decays occurring inside the reactor. A 1 GWth nuclear reactor can generate 21020 e’s/s
en p e
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Sources Are Free
It is true when not including the hidden charge.
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Underground Neutrino Experiments
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How Easy to See a Neutrino?Take the solar neutrino experiment as an example,
targete eN N
Since the solar neutrino flux on the Earth is
10 2 45 27 10 / / , ~ 10
ecm s cm
Assuming a 1kilo ton of water target gives
23 3 3
target
32
(6 10 ) (18 ) / (10 ) /18
~ 10
N molecules e molecule
Thus, the event rate is
~ 0.01/ 1000/e
N s or day
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Why Do We Worry Cosmic Ray?
At sea level, the cosmic flux2
~ 1/ / mincm
That means in 1kilo ton water at sea level, the number of passing thru ’s is
2 1 4~ (10 100) 1min 1.7 10 / s
These ’s can have reactions
1 1 2,
e
N N e
N n X
N N X N N
Mimicking the neutrino reactions.
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How To Reduce Background?
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Underground Labs
China7-7.5km
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Solar Experiments
Radiochemical expts•Homestake (Cl)•Gallex/GNO (Ga)•Sage (Ga)
Č expts•Kamiokande (H2O)•Super-K (H2O)•SNO (D2O)
Scintilator expts•Borexino•KamLAND (?)
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Atmospheric ExperimentsWater Č experiments
•Kamiokande (1000ton)•IMB (3300ton)•Super-K (22.5kton)
Tracking Calorimeter •Nusex (130ton iron)•Frejus (700ton iron)•Soudan (1000ton iron)
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Super Kamiokande Experiment
34
41.4
m
39.3 m 1 km
/e
A 50k tons water Č detector
located at 1k m underground
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Event Classification @ SK
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Expected Flux Distribution
About 13,000 km
About 15 km
-1 0 +1
cos
Going down
Going upFrom other sideof the Earth
From above
same
Expect to see this shape
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Zenith Angle Distributions
DataMC with no oscillationMC with best-fit oscillation
Less deviation for e
Large deviation for
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Oscillation Signature
SK-I,II,III
OscillationDecay (V.D. Barger, et. al)Decoherence (Y. Grossman, et. al)
Neutrino oscillation should have a signature of the
survival probability varying with L/E
Phys.Rev.Lett.93:101801,2004
Alternative models are ruled out at ~5 level
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Tau Neutrino Appearance
2 2 2
max(0, )2
th N NN
N N
m m mmE m
m m
If the deviation is due to
3460.7MeV, 3455.5MeVth th
E E
Then appearance should be
observed. However, in CC
there is a threshold issue
and a short lifetime of ,
complicating the analysis.
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Solar Neutrino Flux
x xe e
8 6 2 1
2005( B) (5.69 0.91) 10 cm s
SSM
8B
hep
ee
e
~15 events/day
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SNO Experiment
Arthur B. McDonald
2092m to Surface1k ton heavy water
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Solar Neutrinos Interactions
SNO only
SNO only
SNO and SK
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First Result from SNO
Good agreement between the measurement and the SSM.
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Three Phases Of SNO
S. Oser
Efficient detection of the neutrons produced via the NCplays a key role in measuring the solar neutrinos.
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Final Answer from SNO
8 6 2 1
2005( B) (5.69 0.91) 10 cm s
SSM
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KamLAND ExperimentObservation of the reactor neutrino disappearance at L/E value where the solar neutrino effect occurs
13m
18m
Located at Kamioka, using 1k ton liquid scintillator as the target.
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Reactor Neutrinos at KamLAND
Japan reactors 94~97%
Korea reactors 3 ~ 5%
world reactors ~ 0.5%
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First Result From KamLAND
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Latest Results From KamLAND
2 0.14 0.15 5 2
21 0.13 0.15
2 0.10 0.10
12 0.07 0.06
Δ 7.58 (stat) (syst) 10 eV
tan 0.56 (stat) (syst)
m
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Borexino Experiment
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7Be Solar Neutrino Measurement
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Impact from Borexino
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Comparison With Solar Models
• Borexino measurement:
49 ± 3(stat) ± 4 (syst) cpd/ 100ton
• High metallicity Solar model MSW/LMA:
48 ± 4 cpd / 100ton
• Low metallicity Solar model , MSW/LMA
44 ± 4 cpd / 100ton
• High metallicity Solar model, nonoscillatingneutrino (inconsistent with measurement at the 4 σ C.L.)
74 ± 4 cpd / 100ton
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Achievement on Mass Splitting and Mixing Measurements
PDG1995
PDG1999
PDG2004 PDG2008
2 2 2Δ :Δ or Δ or Δ ; : or or
atm LSND atm LSNDm m m m
Dark Age
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Do We Fully Understand Neutrino Oscillation Now?
12 23,
atm
,e
13
1 2 3 3 1 2
?
or ?m m m m m m
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Search For Non-Zero 13 In Non-Accelerator Neutrino
Experiments
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Why Is It So Important?
sinc
si
os
osn c
1
2
13
12
13
13
0 0 0
0 1 0 0 0
0 0 0 1
ii
i
i
e e
e
e
CP violation parameters:
Since 13 is the gateway of CP violation in lepton sector!
Majorana phases 1, 2 (very hard)
Dirac phase (may be accessible thru accelerator
neutrino experiment provided that sin13 is not so
small)
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Current knowledge on 13Direct search (PRD 62, 072002) Global fit (hep-ph/0905.3549)
A small 13(e.g. sin2213<0.01) would make future experimental
searches for CP violation become a kind of “Mission: Impossible”.
At m231 = 2.5 103 eV2,
sin22 < 0.17
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Theoretical predictions for 13
A precise 13 measurement is helpful in understanding
the physics beyond the Standard Model.
Excluded region
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How to measure 13?Disappearance searches at reactors:
Appearance searches at accelerators:
Reactor experiments provide a clean environment to measure 13.
Accelerator experiments give access to both 13 and values.
13
2 2 2 2
12 13 31
2 2 2
4 2 2 2
12 13 12
2
12 13 3
21
2
cos sin 2 sin (1.267 )
sin sin 2 sin (1.2
cos sin 2 sin (1.26
67 )
7 )dis
P
Lm
E
P m
L
E
L
E
m
P
22 2 2 2 2 2 2
23 23 23 113
2
1
2
1
2
3 3
1sin sin (1.267 ) cos sin sin (1.26sin
cos s( sinin
)
)
7app
L Lm m
A
E EP
2
13sin 2 0.1
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How to Reach 1% Precision?
Increase statistics: Need intensive neutrino flux from powerful nuclear reactors
Utilize larger target mass, hence larger detectors
Reduce systematic uncertainties: Reactor-related:
Optimize baseline for best sensitivity and smaller residual errors
Near and far detectors to minimize reactor-related errors
Detector-related:
Use “Identical” pairs of detectors to do relative measurement
Comprehensive program in calibration/monitoring of detectors
Interchange near and far detectors (optional)
Background-related
Go deeper to reduce cosmic-induced backgrounds Enough active and passive shielding
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The Detector Place Selection
e
Near
Far
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Signature of A Signal
0
0
( >2 =1.022MeV)
Reaction:
Prompt signal:
Delayed signal: ( ~ 8MeV, ~ 28 )
( 2.2MeV, ~ 1
2 '
80 )Delayed signal
'
:
e
ee
e n
e
n
p
E m
G
e
Gd d E s
s
n d
s
E sp
Neutrino energy:
epnne
mMMTTE )(
Threshold=1.8 MeV
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Reactor Experiments
Double Chooz, France
Expected sin2213~0.03
85 ton-GWth
Small UK interest
(Sussex, no longer funded)
Daya Bay, China
Expected sin2213~0.01
1400 ton-GWth
RENO, Korea
Expected sin2213~0.03
250 ton-GWth
Main differences:
• Reactor power/no of cores
• Configuration cores vs. detectors; no. of detectors
• Detector target mass
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Status and Expected Milestones
2009
2010
2011
2012
2013
2014
2009
2010
2011
2012
2013
2014
2009
2010
2011
2012
2013
2014
Double Chooz RENO Daya Bay
ND and FD readyfor data-taking
N and F tunnelscompleted
ND and FD commissioning
sin2 213 ~ 0.03 ???
First detector complete; start dry run
Near Hall ready for data-taking
Far Hall ready for data-taking;Ling Ao Hall ready abit earlier
Near Hall occupancy
sin2 213 ~ 0.01
FD ready for data-taking
sin2 213 ~ 0.06
ND ready fordata-taking
sin2 213 ~ 0.03
ND hall + tunnelconstruction begins
Near : 1,280/dayFar : 114/day
Near : 1,680/day (DYB)1,480/day (LA)
Far : 360/dayNear : 500/dayFar : 50/day
Elisabeth Falk
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Expected SensitivitiesHuber et al. arXiv:0907.1896
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DayaBay Civil Construction
Daya BayReactors
Ling AoReactors
Liquid Scintillator
hall
Ling Ao IIReactors
Entrance
Construction tunnel
Waterhall
Daya Bay Near
Far site
Ling Ao Near
As of late September…
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Waiting for 13
Double-Chooz, DayaBay, RENO, T2K, …Which one will win the game?
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Future Prospects for Non-Accelerator Neutrino
Experiments
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Work-To-Do and Remaining Issues
Precise measurements of (m23)2 and (sin223)2 (atmospheric neutrino experiments)
Solar neutrino oscillation in the transition phase between vacuum effect and matter effect (solar neutrino experiments)
Measurement of 13 (reactor experiments)
CP violation and mass hierarchy (need to collaborate with accelerator experiments)
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Atmospheric Future Prospect
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Solar Neutrino Future Prospects
Borexino Super-Kamiokande IV SAGE KamLAND LENS SNO+ CELAN MOON XMASS
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Reactor Neutrino Future Prospects
For 13
Double-CHOOZ DayaBay RENO
For 12
DayaBay II (60km)?
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Summary
• Compelling evidences for neutrino oscillation from– Atmospheric neutrino experiments– Solar neutrino experiments– Reactor antineutrino experiment– Accelerator neutrino experiments (yesterday lecture)
• Neutrino oscillation indicates new physics (NP) beyond the Standard Model, but we still don’t know what NP is yet.
• Measuring non-zero 13 is the priority task for non-accelerator neutrino experiments.