past neutrino mass & oscillations present atmospheric neutrinos solar neutrinos future
DESCRIPTION
Solar & Atmospheric Oscillation Experiments Greg Sullivan University of Maryland Aspen Winter Conference January 21, 1999. Past Neutrino Mass & Oscillations Present Atmospheric neutrinos Solar neutrinos Future. n. ??. e. Can we detect them? - PowerPoint PPT PresentationTRANSCRIPT
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Solar & Atmospheric Oscillation Experiments
Greg Sullivan University of Maryland
Aspen Winter ConferenceJanuary 21, 1999
PastNeutrino Mass & Oscillations
PresentAtmospheric neutrinosSolar neutrinos
Future
PastNeutrino Mass & Oscillations
PresentAtmospheric neutrinosSolar neutrinos
Future
??
e
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Can we detect them?In 1934 Bethe & Peierls calculated the
cross section for neutrino interaction of 10-44 cm2.
Nature (London) 133, 532(1934)
“It is therefore absolutely impossible to observe processes of this kind with neutrinos created in nuclear transformations”
“… one can conclude that there is no practically possible way of observing the neutrino.”
“… and it is not necessary to assume interaction in order to explain the function of the neutrino nuclear transformations ...”
In fact, it was some 20 years before they were detected using a nuclear reactor as a source.
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Solar Neutrino Spectrum
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Solar Neutrinos detected R. Davis and his 37Cl detector
same principle used to try and detect antineutrinos from a nuclear reactor in 1955.
measured the flux of neutrinos from the sun almost continuously since about 1970!
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Solar Neutrino Rate in Cl Detector is 1/3-1/2 expected
Astrophysics - Standard Solar ModelNeutrinos from 7Be and 8BVery sensitive to Sun’s core temperature
Particle Physics Solutions --- Neutrino properties are not what we think!
Electron Neutrinos don’t make it to earthMagnetic properties of e change flavor in transit - Neutrino
Oscillations!Non zero neutrino mass!Lepton flavor mixing!
Explanations?
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Neutrino Mass & Neutrino Oscillations? What is the mass of the neutrino?
Is it identically zero?If not, Why is it so small?
see-saw mechanism
T h e m o s t g e n e r a l m a s s L a g r a n g i a n f o r o n e n e u t r i n o f l a v o r i s :
L m m m h cm D L R R L L Lc
L R Rc
R . .
w h e r e m D , m L , m R r e p r e s e n t t h e D i r a c , l e f t - h a n d e d M a j o r a n aa n d r i g h t - h a n d e d M a j o r a n a m a s s e s . T h i s c a n b e w r i t t e n i nm a t r i x f o r m a s :
L S M Sm
w h e r e ,
S
Mm m
m m
L Lc
R Rc
L D
D R
T h e p h y s i c a l m a s s e i g e n s t a t e s a r e f o u n d b y d i a g o n a l i z i n g t h em a s s m a t r i x . I f w e a s s u m e m L = 0 w e g e t :
mm m
mR D
R1 2
2
221 1
4,
F o r a h e a v y r i g h t - h a n d e d s c a l e m R > > m D , w e g e t t w o m a s se i g e n s t a t e s
m m h e a v y M e V m
mm
ml i g h t s e V
H R W
D
R
( )
( ) '
5 0 5 0 0
1 0 1 02
6
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Neutrino Oscillations If mass is not 0 and flavor is not absolutely
conserved then “mixing” may occur between different type of neutrinos. Weak eigenstates of the neutrino are mixtures of the neutrinos with definite mass.
F o r t w o n e u t r i n o s p e c i e s e a n d w e h a v e :
cossin
sincos
21
21
e
w h e r e a n d 2 a r e t h e m a s s e i g e n s t a t e s .
I n a w e a k d e c a y o n e p r o d u c e s a d e f i n i t e w e a k e i g e n s t a t e
t e 0 .
.A t a l a t e r t i m e t h e p r o b a b i l i t y o f t h e f i n a l s t a t e w i l l b e :
sincos 2121
tiEtiE eet
T h e s u r v i v a l p r o b a b i l i t y i s :
GeV
kmeVee E
LmLP
222 27.1
ins2sin1; .
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Solar Neutrino Experiments
Homestake - RadiochemicalHuge tank of Cleaning Fluid
e + 37Cl e- + 37Ar
Mostly 8B neutrinos + some 7Be30 years at <0.5 ev/day1/3 SSM
Sage/Gallex - Radiochemical“All” neutrinos
e + 71Ga e- + 71Ge
4 years at ~0.75 ev /day~2/3 SSM
Kamiokande-II and -III 8B neutrinos only
e Elastic Scattering
10 years at 0.44 ev /day~1/2 SSM
Homestake - RadiochemicalHuge tank of Cleaning Fluid
e + 37Cl e- + 37Ar
Mostly 8B neutrinos + some 7Be30 years at <0.5 ev/day1/3 SSM
Sage/Gallex - Radiochemical“All” neutrinos
e + 71Ga e- + 71Ge
4 years at ~0.75 ev /day~2/3 SSM
Kamiokande-II and -III 8B neutrinos only
e Elastic Scattering
10 years at 0.44 ev /day~1/2 SSM
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Summary of Results Before Super-K
Four experiments measured versus predicted from solar model
Four experiments measured versus predicted from solar model
Experiment SSM(BP92) DATA DATA/SSM
GALLEX (Ga)
132 7 70 8 0.54
SAGE (Ga)
“ 73 11
Homestake (Cl)
8 1.1 2.55 .25 0.32
Kamioka (H2O)
5.7 .8 2.80 .38 0.49
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FROM Langacker -Allowed regions at 95% CL from individual experiments and from the global fit. The Earth effect is included for both time-averaged and day/night asymmetry data, full astrophysical and nuclear physics uncertainties and their correlations are accounted for, and a joint statistical analysis is carried out. The region excluded by the Kamiokande absence of the day/night effect is also indicated.
BP95
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Atmospheric Neutrinos
Absolute Flux Predicted to ~20% :
• primary CR spectrum
• geomagnetic cutoff
• hadron production modeled from accelerator data
2
ee
Ratio predicted to ~ 5%
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Atmospheric Neutrino Anomaly
The Observed Ratio of /e is too lowProduced when pions generated in the upper
atmosphere by cosmic rays decay.
Predicted Ratio of /e ~ 2
Observed Ratio is ~ 1
Particle Physics Solutions --- Neutrino properties are not what we think!
Muon Neutrinos don’t make it to earth
change flavor in transit - Neutrino Oscillations!
Non zero neutrino mass!Lepton flavor mixing!
ee
XNP
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Worldwide Results on “R”Before Super-Kamiokande
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Two Suggestions of Neutrino Transformation
Solar Neutrinos (~1-15 Mev e)Davis experiment (Cl) saw ~30% of expected
flux of e from 8B & 7Be
Galium experiments showed less than
expected flux of e from all processes
Kamiokande saw ~40% e from 8B
These results can not be reconciled with the standard solar model
Atmospheric Neutrinos (~.1 - 3 GeV) IMB and Kamiokande saw less than
expected ratio of e
One Proposed Explanation was: Neutrino Oscillations
Solar neutrinos might be e
Atmos. neutrinos might be
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Super-Kamiokande The Next generation Underground Neutrino Detector.
Detector Characteristics41 m h x 39 m dia.50,000 tonne total/22,000 tonne fiducial11,200 20” PMTs inner detector1,850 8” PMTs anti-detector40% photocathode coverage
Trigger Threshold ~5 MeV Resolution
Energy 16%/(E)1/2 at 10 MeVPosition ~50 cm at 10 MeVAngular ~30 degrees at 10 MeV
Super-Kamiokande is a 50,000 ton water Cerenkov detector at a depth of 1000 meters in the Kamioka Mozumi mine in Japan.
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SuperKamiokandeCollaboration
Institute for Cosmic Ray Research, University of Tokyo Gifu University Institute for Nuclear Study, University of Tokyo National Laboratory for High Energy Physics, KEK Kobe University Miyagi Education University Niigata University Osaka University Tokai University Tohoku University Tokyo Institute of Technology Boston University Brookhaven National Laboratory University of California, Irvine California State University, Dominguez Hills Cleveland State University George Mason University University of Hawaii Los Alamos National Laboratory Louisiana State University University of Maryland State University of New York, Stony Brook University of Warsaw University of Washington
Institute for Cosmic Ray Research, University of Tokyo Gifu University Institute for Nuclear Study, University of Tokyo National Laboratory for High Energy Physics, KEK Kobe University Miyagi Education University Niigata University Osaka University Tokai University Tohoku University Tokyo Institute of Technology Boston University Brookhaven National Laboratory University of California, Irvine California State University, Dominguez Hills Cleveland State University George Mason University University of Hawaii Los Alamos National Laboratory Louisiana State University University of Maryland State University of New York, Stony Brook University of Warsaw University of Washington
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The Super-K Detector
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The Super-Kamiokande Tank During Filling in 1996
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Stopping Muon
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Electron from decay of stopping muon
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Muon - Electron Identification
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Sub-Gev (535 days)
Evis < 1.33 GeVPe > 100 MeV/cP> 200 MeV/c
Data MC
1 Ring
e-like 1231 1049
-like 1158 1574
Multi-ring 911 981
)(05.)(026.63.0
/
/syststat
e
e
MC
Data
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Multi-Gev (535 days)
Evis > 1.33 GeV
Data MC
1 Ring
e-like 290 236 -like 230 297Multi-ring 533 560
)(08.)(05.65.0
/
/syststat
e
e
MC
Data
Fully Contained
Data MC
Total =-like
301 372
Partially Contained
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Worldwide Results on “R”
Detectors continue to runMACRO upward going muonsSoudan IISuper-K muons
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If the muon ‘s oscillate, what it look like?
Depletion of relative to e
“double ratio” R
L dependence of flux
Zenith angle dependence
1
/
/
MC
data
e
eR
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Zenith Angle Dependence
Survival Probability vs. Distance (1GeV,.003 eV^2)
0
0.25
0.5
0.75
1
10 100 1000 10000
Distance (km)
Pro
ba
bil
ity
GeV
km
E
LmLP
222 27.1
sin2sin1;
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Zenith Angle Dependence
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Zenith Angle Dependence
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L/E Distribution of Atmospheric Neutrinos
The dashed lines show the expected shape for at m2=2.2 x 10-3 eV2 and sin2 2 = 1.
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Atmospheric Results
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East-West Effect
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Zenith Angle Distribution(736 Day Sample)
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Zenith Angle Dependence(736 day sample)
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MACRO Detector
Data collected ‘89 - Dec ‘97~3 live-years with 6 full SM~480 Upward Going Muon events
R(data/MC)= 0.74 .036sta.046sys.13theo
Probability for no oscillations
P(null) = 14%Best fit mass assuming maximal mixing:
m2 ~ 2 x 10-3 eV2
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MACRO upward-going muons
Probabilities Number + ShapeProbability of no oscillations
P(null) 0.1%Best fit oscillation parameters
sin22 = 1.0 , m2 2 x 10-3 eV2
P(best fit) 17%
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A Picture of the Sun using Neutrinos in Super-K
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10 MeV Electron in Super-K
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Super Low Energy (SLE) Data
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Solar Neutrino Flux(New 708 Day Sample)
)(013.0)(008.0471.098
syststatSSM
Data
BP
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Day-Night Results708 day Sample
)(013.0)(016.0026.0 syststatND
ND
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Energy Spectrum708 day + 419 day SLE
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Spectrum and Oscillations?
Data favors Vacuum solution (red)small angle MSW (blue) starting to get
squeezed by flatness with SLE data
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Hep Neutrinos ? Set limit on hep flux from data
integral of events between Ethres & Eend
Ethres= 17 MeV , Eend= 25MeV
Hep flux < 8 SSM at 90% C.L.Ethres= 19 MeV , Eend= 20 MeV
Hep flux < 20 SSM at 90% C.L.
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Seasonal Variation
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Energy Dependence of Seasonal Variation for Just-so solution
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Seasonal Variation in High Energy Data
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Summary of Super-K Results
Atmospheric Neutrinos
Strong Evidence for s) Oscillations
New results consistentHigher statistics may allow separation of
(s)
Solar NeutrinosNo evidence for Day/Night Effect
Squeezes Large Angle SolutionSuper Low E and more statistics
somewhat flattens energy spectrumStarting Squeeze Small Angle
SolutionVacuum (Just-So) solution is still aliveContinue to Run
Postponed the scheduled June ‘99 shutdown
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Future ~2000
Atmospheric NeutrinosContinued running of Super-Kamiokande
Neutral Currents ?Distinguish from s
MACRO muons & neutrinosSoudan IIKEK to Super-K (K2K)
Solar NeutrinosSpectral Distortion at High EnergyInstrumental Effect?
Energy Scale & Resolution
LINAC limitationsD-T Generator to make 16N as
calibration source (NSF)Hep Neutrinos?
Need 20 times predicted fluxUse Super-K data >18 MeV to set limit
on hep flux??Statistics?Seasonal Variation needs more data
Atmospheric NeutrinosContinued running of Super-Kamiokande
Neutral Currents ?Distinguish from s
MACRO muons & neutrinosSoudan IIKEK to Super-K (K2K)
Solar NeutrinosSpectral Distortion at High EnergyInstrumental Effect?
Energy Scale & Resolution
LINAC limitationsD-T Generator to make 16N as
calibration source (NSF)Hep Neutrinos?
Need 20 times predicted fluxUse Super-K data >18 MeV to set limit
on hep flux??Statistics?Seasonal Variation needs more data
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Future 2000+
Atmospheric NeutrinosAccelerator Experiments (FNAL, CERN,
KEK)Known Neutrino DirectionBetter Neutrino Energy Measurement
Appearance Experiment ??
Solar Neutrinos Continued Super-Kamiokande RunningNew Experiments Soon - should settle the
solar neutrino problemSudbury Neutrino Observatory (SNO)
Canada,US,UK 11 institutions Fill Apr, 98 -- Feb, 99 ?6 mo. Debug & Calibration1 Yr. pure D2O
BorexinoICARUS
Atmospheric NeutrinosAccelerator Experiments (FNAL, CERN,
KEK)Known Neutrino DirectionBetter Neutrino Energy Measurement
Appearance Experiment ??
Solar Neutrinos Continued Super-Kamiokande RunningNew Experiments Soon - should settle the
solar neutrino problemSudbury Neutrino Observatory (SNO)
Canada,US,UK 11 institutions Fill Apr, 98 -- Feb, 99 ?6 mo. Debug & Calibration1 Yr. pure D2O
BorexinoICARUS
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SNO Detector
Detector PerformanceThreshold 5MeV - 8B neutrinosEnergy Resolution 14% at 10 MeVCharged Current off D - 26.7 ev/day
measure NEUTRINO energy
- look for spectral distortion with high sensitivity
- seasonal variation over entire spectrumNeutral Current 7.7 ev/day
CC/NC ratio “smoking gun”Electron Scattering 3.0 ev/day
-1000 tonnes of D2O
-6800 feet Underground
-10,000 pmts
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SNO Sensitivity
1) CC/NC Ratio
2) Spectrum
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Borexino
Detector PerformanceElectron Threshold low enough to
observe 7Be (863 keV) neutrinosReal time measurement of 7Be & 8B46 events/day in 100 ton fiducial volumeFirst Measurement of only the 7Be flux
final ingredient
-300 Tonnes of Scintillator
-2200 Pmt’s
-Gran Sasso
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Solar Neutrinos in Near Future
PossibleSolutions
*
Super-K(Boron)
SNO(Boron)
Borexino(Be)*
Boone(Acc)
NoSolarOsc
Flux lowNo specNo D/NNo Seas
Flux low?No SpecCC/NCOK
Meas/exp
1Possible
signal
SmallAngleMSW
SpectralDistortion?
SpectrumCC/NClow
~1/4 NoSignal
LargeAngleMSW
Day/NightDay/NightCC/NClow
~1/2 NoSignal
VacuumOsc Spectrum
Season?
SpectrumSeasonCC/NClow
~1/2 NoSignal
SmallAngleSterile
Spectrum?SpectrumCC/NCOK
~.01 Possiblesignal
*Bahcall Phys Rev D 58
(http://www.sns.ias.edu/~jnb/)
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Atmospheric NeutrinoOscillations
Need Confirmation of EvidenceFurther Running of Super-k, Soudan,
MACROAccelerator Experiments planned
MINOS at FNALCERN to Gran Sasso
- Disappearance experiments?
Future PossibilitiesMegaton underground Atmospheric
Neutrino detector
Appearance Experiment?5 GeV Neutrinos L/E ~ 1 x 103
L ~ 5000 km