Solar Neutrino Physics
description
Transcript of Solar Neutrino Physics
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Solar Neutrino Physics
Aksel HallinPIC 2010
University of Alberta
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Solar Neutrino Physics
• Neutrino Physics (the sun is a very intense and quite well understood source of neutrinos)– Neutrino Oscillations – Non standard neutrino interactions
• Solar Physics (understanding the details of the neutrino flux)– Do we understand fusion inside the sun?
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Solar Neutrino Problem
Either
Solar Models are Incomplete or Incorrect
Or
Neutrinos undergo Flavor Changing Oscillations or other new physics.
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Radiochemical : Cl, GaGa rate: 66.1 ±3.1 SNU SAGE+GNO/GALLEX [PRC80, 015807(2009)]Cl rate: 2.56 ±0.23 SNU [Astrophys. J. 496 (1998) 505]
SKSK-I 1496 days, with the zenith spectrum E > 5.0 MeVThere is in total 5 day bins and 6 night bins (mantle 1,2,3,4,5 and core) 8B flux: 2.35 +- 0.02(stat) +- 0.08(syst) [x 106 /cm2/sec]A(day/night) = -0.021 +- 0.020(stat) +0.013 -0.012(syst)SK-II 791 days, spectrum + D/N E > 7.5 MeV It corresponds to:8B flux 2.38 +- 0.05(stat.) +0.16 -0.15(syst) [x 106 /cm2/sec]A(day/night) 0.063 +- 0.042(stat) +- 0.037(syst)
Borexino7Be rate: 49 ± 5 cpd/100tons [PRL101, 091302(2008)]
KamLAND reactor experiment: 2008 results [PRL100, 221803 (2008)]8B spectrum: W. T. Winter et al., PRC 73, 025503 (2006).SSM for the contours: BS05(OP).
New Borexino result PRD 82, 033006(2010): 3MeV threshold!
8
6 2 12.4 0.4 0.1 10 cm sES
B
Status of the Field
+ SNO (this talk)
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Solar n Measurements Global Summary
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Status of the Field (continued)
• Solar Experiments (and Kamland) are all consistent with SSM+ 2 flavour MSW oscillations, no short term solar variability and with parameters
8
0.119 6 2 10.148
2 0.04012 0.029
2 0.20 5 221 0.21
5.013 10 cm s
tan 0.457
7.59 10 eV
B
m
Theoretical Uncertainty ~15%
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Results of fit: 2 flavour oscillation analysis
SNO only
FIG. 38: (Color) Two-flavor oscillation parameter analysis for a) global solar data and b) global solar + KamLAND data. The solar data includes: SNO’s LETA survival probability day/night curves; SNO Phase III integral rates; Cl; SAGE; Gallex/GNO; Borexino; SK-I zenith and SK-II day/night spectra.
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Neutrino Oscillations
1 2
Flavour Eigenstates: ,
Mass Eigenstates: ,e x
1
2
cos sin
sin cose
x
2 2
2 2
cos2 sin 21 2 22
sin 2 cos22 2
e e
x x
m md E Eidt m m
E E
1
e
2x
The time evolution is written in terms of the mass matrix, the neutrino energy E and the mass difference
2 21 sin 2 sine
xP
L
2
2
eV2.48
1 MeV
EL m
m
The survival probability of an electron neutrino in terms of the distance travelled, x, andvacuum oscillation length L is:
2 2 22 1m m m
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Matter Enhanced Flavour Oscillations (the MSW effect)
2 2
2 2
cos2 2 sin 21 2 22
sin 2 cos2 22 2
F ee e
x xF e
m mG n
d E Eidt m m
G nE E
Within matter, the electron neutrino interacts with electrons with a charged current interaction. All neutrinos can interact with the neutral current interaction. The additional interaction contributes an additional term to the electron neutrino Hamiltonian
2
cos2 22 F e
mG n
EThe resonance condition occurs when :
In that case, neutrinos can undergo complete conversion from one flavour to another.
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New Physics/Measurements
• Precision measurements of 8B (SNO 3 phase), pep (Borexino, SNO+), hep (SNO- part of 3 phase analysis), CNO (SNO+), pp fluxes
• sin2θ13 <0.057 from 3 neutrino fits to Solar+Kamland
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2 vs 3 flavour oscillations
Float Boron-8 flux, and Θ13
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3 Phase analysis
2 2.09 2 213 1.63 13sin 2.00 10 sin 0.057(95% C.L.)
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Low Energy Solar Neutrinos
p + p 2H + e+ + e p + e− + p 2H + e
2H + p 3He +
3He + 3He 4He + 2 p 3He + p 4He + e+ + e
3He + 4He 7Be +
7Be + e− 7Li + + e7Be + p 8B +
7Li + p + 8B 2 + e+ + e
p-p Solar Fusion Chain
• complete our understanding of neutrinos from the Sun
pep, CNO, 7Be, pp
17
CNO Cycle
12C + p → 13N + g 13N → 13C + e+ + ne
13C + p → 14N + g14N + p → 15O + g 15O → 15N + e+ + ne
15N + p → 12C + a
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18
Adapted from N
OW
2009,Ludhova
pep expectation
0.2
0.3
0.4
0.5
0.6
0.7
0.1 1 10Neutrino Energy (MeV)
Friedland, Lunardini, Peña-GarayPhys Lett B 594 347-354 (2004)
Compare with (previously shown) NSI expectations:
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pep neutrinos
Depth makes this experiment easier:SNO+ (6080 mwe), this is • 100 times better than Borexino (3500 mwe), • 600 times better than KamLAND (2700 mwe)
21 Sep 2009 19
Pee for pep is very sensitive to NSI
Borexino Collaboration, Phys.Rev. Lett. 101, 091302 (2008) e
Sur
viva
l Pro
babi
lity,
Pee
0.2
0.3
0.4
0.5
0.6
0.7
0.1 1 10Neutrino Energy (MeV)
Non-StandardInteractions
StandardModel
Frie
dlan
d, L
unar
dini
, Peñ
a-G
aray
Phys
Lett
B 5
94 3
47-3
54 (2
004)
LMA-0 pepLMA-0 8B LMA-1 8B
LMA-1 pep
pp pep7Be 8BSNO
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Solar opacity problemIncompatible with helioseismology
measurements:
21 Sep 2009 20 High Z Low Z
Improved 3D hydrodynamic modeling (Asplund, Grevesse and Sauval, 2005)of result in lower Z by a factor of almost 2!
arXiv:0811.2424
core
However, this does not fit well with helioseismology either. (Castor et. al. astro-ph/0611619)
Possible solution: (see Haxton and Serenelli, Ap. J. 687, 678 (2008))
core is different than the convective zone (opacity).
probe solar core with neutrinos
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Faint young sun “paradox”
21
Bahcall, Pinsonneault, Basu, THE ASTROPHYSICAL JOURNAL, 555:990È1012, 2001 July 10
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Sudbury Neutrino Observatory
1700 tonnes Inner
Shielding H2O
1000 tonnes D2O$300 M
5300 tonnes Outer
Shield H2O
12 m Diameter Acrylic Vessel
Support Structure for 9500 PMTs, 60% coverage
Urylon Liner and
Radon Seal
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Neutrino-Electron Scattering (ES). 3/day SSM; 1.35/d LETA
Charged Current (CC): 24/day SSM; 6.6/day LETA
Neutral Current (NC): 9.22/d SSM; 8.32/d LETA
Neutrino-deuterium reactions
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Observables
-position-time-charge
Reconstructed event-vertex-direction-energy-isotropy
Photomultiplier tube
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Phase I: Just D2O: neutron capture on deuterium• Simple detector configuration, clean measurement• Low neutron sensitivity• Poor discrimination between neutrons and electrons
Phase II: D2O + NaCl: neutron capture on Chlorine• Very good neutron sensitivity• Better neutron electron separation
• Phase III: D2O + 3He Proportional Counters• Good neutron sensitivity• Great neutron/electron separation
Three Phases of SNO: 3 NC reactions
; 6.3 MeVn d t E
35 36Cl Cl+ ; 8.6 MeVn E
3 He p+tn
Nov. 1999-May 2001
June 2001-Sept 2003
Jan 2004-Nov. 2006
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Backgrounds drive Design
g’s over 2.2 MeV d + g n + p
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Analysis
• Data cleaning to remove instrumental backgrounds (cuts developed on subset of data; tested with MC and sources)
• Calibrations: wide array of sources. Laserball was used for primary calibration (determining optical parameters for MC). N16 was used to determine absolute QE of pmt’s. 25% of our running time spent calibrating
• Large number of parameters in MC. Use the difference between calibration sources and MC to quantify systematic uncertainties.
• Blind and multiple analyses
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The best analysis to date is the so-called LETA (low energy threshold) analysis
(PRC 81 055504, 2010)
Joint Phase I+II down to Teff>3.5 MeVSignificantly reduced systematicsDirect ne survival probability fit
SNO trigger threshold <~2.0 MeV for all phases
Previous SNO analysis thresholds: T>5.0 MeV/5.5 MeV/6.0 MeV Phase I/II/III
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Advantages of Low Threshold Analysis
En=6 MeV En=6 MeV
ne Statistics
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Phase I (D2O) NC
+74%
+68%
Advantages of Low Threshold Analysis nx (NC) Statistics
Phase II (D2O+NaCl)
NC
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Phase I (D2O)
Phase II(D2O+Salt)
“Beam On”
“Beam Off”
Advantages of (2-Phase) Low Threshold Analysis Breaking NC/CC Covariance
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Teff>3.5 MeV
Challenges of a Low Threshold MeasurementCosmic rays < 3/hour
All events (before background reduction);
~5000 ns
Low Energy Backgrounds
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3 neutrino signals+ 17 backgrounds
Kinetic Energy Spectrum
New Threshold = 3.5 MeV
MC
Challenges of a Low Threshold Measurement
PMT -b gs
internal (D2O)
external (AV + H2O)
NC+CC+ES (Phase II)
Old threshold
Low Energy Backgrounds
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How Do We Make a Low Threshold Measurement?
To make a meaningful measurement, we:• Reduced backgrounds• Reduced systematic uncertainties • Fit for all signals and remaining backgrounds
Entire analysis chain re-done, from charge pedestals to simulation upgrades to final `signal extraction’ fits
Primary reasons for improvement in precision:1. Increased statistics2. Breaking of NC/CC covariance3. Reduction in systematic uncertainties
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Low Energy Threshold AnalysisSignal Extraction Fit (Signal PDFs)
Not used
1 D projections
Teff (MeV) cosqsun
(R/RAV)3
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Low Energy Threshold AnalysisSignal Extraction Fit (3 Background PDFs)
1 D projections
Teff (MeV) cosqsun
(R/RAV)3
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1. Maximum likelihood with binned pdfs: Manual scan of likelihood space (iterative)
• Locate best fit and +/- 1s uncertainty data helps constrain systematics
• `human intensive’2. Kernel estimation---ML with unbinned pdfs:
Low Energy Threshold AnalysisSignal Extraction Fit
(3 signals+17 backgrounds)x2, and pdfs are multidimensional:
ES, CC
NC, backgrounds
Two distinct methods:
•Allows full `floating’ of systematics, incl. resolutions
• CPU intensive---use graphics card!
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Background Reduction
Low Energy Threshold Analysis
New energy estimator includes both `prompt’ and `late’ light
12% more hits≈6% narrowing of resolution~60% reduction of internal backgrounds
New Cuts help reduce external backgrounds by ~80%
Fiducial Volume
βγβ
High charge early in timeExample:
Rayleigh Scatter
(it was good we fixed our pedestals…)
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Low Energy Threshold AnalysisSystematic Uncertainties
• Nearly all systematic uncertainties from calibration data-MC• Upgrades to MC simulation yielded many reductions• Residual offsets used as corrections w/ add`l uncertainties• All uncertainties verified with multiple calibration sources
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Laserball Calibration
dij d aij a hij hd a d a d a
ij i ij ij ij ij jN N R T L e
Insert laserball in typically 30 positions, at each of 6 wavelengths (337,365,386,420,500,620) nm; measure the number of prompt photons in each run i for pmt j; typically about 250,000 measurements per scan. Fit an optical model to determine parameters in MC.
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Improved low level response of PMTs in MC
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Volume-weighted uncertainties: Old: Phase I = ±1.2% Phase II = ±1.1% New: Phase I = ±0.6% Phase II = ±0.5% (about half Phase-correlated)
Low Energy Threshold AnalysisSystematic Uncertainties—Energy Scale
No correction With correction
16N calibration source6.13 MeV gs
Tested with: Independent 16N data, n capture events, Rn `spike’ events…
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Central runs remove source positioning offsets,
MC upgrades reduce shifts
Fiducial volume uncertainties: Old: Phase I ~ ±3% Phase II ~ ±3% New: Phase I ~ ±1% Phase II ~ ±0.6%
Low Energy Threshold AnalysisSystematic Uncertainties—Position
Tested with: neutron captures, 8Li, outside-signal-box ns
Old New
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Low Energy Threshold AnalysisSystematic Uncertainties—Isotropy (b14)
MC simulation upgrades provide biggest source of improvementTests with muon `followers’, Am-Be source, Rn spike
b14 Scale uncertainties: Old: Phase I --- , Phase II = ±0.85% electrons, ±0.48% neutrons New: Phase I ±0.42%, Phase II =±0.24% electrons,+0.38%
-0.22% neutrons
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PassFail
FailPass
FailFail
PassPass
NPF = e1(1-e2)Nb
NFP = (1-e1) e2Nb
NFF = (1-e1)(1-e2)Nb
NPP = e1e2Nb + Ns
NPMT= NPP – Ns = NFP * NPF /
NFF
Low Energy Threshold AnalysisPMT -b g PDFs
Not enough CPUs to simulate sample of events Use data instead
In-time ratio In-time ratio
Early
cha
rge
prob
abili
ty
Early
cha
rge
prob
abili
ty
(so fixing pedestals gave us a handle on these bkds…)
`Bifurcated’ analysis
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Low Energy Threshold Analysis Analysis Summary
• Fits are maximum likelihood in multiple dimensions (two methods)• Most PDFs generated with simulation• Systematics from data-MC comparisons• In some cases, corrections applied to MC PDFS based on comps.• Tested on multiple independent data sets
•
• PMT pdf generated from bifurcated analysis of data• Tested on MC and with independent analysis using direction vs. R3
• Dominant systematics (6/20) allowed to vary in fit• Constrained by calib.• Note: many backgrounds look alike! But very few look like signal• Some backgrounds have ex-situ constraints from radiochm. assays
208Tl
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Results of Fit: NC0.159 0.132 6 2 10.158 0.1145.171 (stat) (syst) 10 cm s
6 2 1cf BP2005: 5.69 10 cm s
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Results of Fit: CC and ES spectra
2 21.5 /15
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Results of fit: 1D projections
Phase 1 Phase 2
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2 and 3 flavour fits
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Future SNO Publications• High frequency periodicity studies (solar g-modes)• Burst searches• Exotics (e.g., n-nbar oscillation)• 3-Phase analysis including NCD pulse shape analysis and hep analysis
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SNOLAB Construction: Started 2005; now complete
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Conclusion:
• Solar Experiments (and Kamland) are all consistent with SSM+ 2 flavour MSW oscillations, no short term solar variability and with parameters
8
0.119 6 2 10.148
2 0.04012 0.029
2 0.20 5 221 0.21
5.013 10 cm s
tan 0.457
7.59 10 eV
B
m
Theoretical Uncertainty ~15%
But the story is not over for solar and neutrino physics…
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Ended data taking 28 Nov 2006 Most heavy water returned June 2007 Finish decommissioning end of 2007
55
SNO
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SNO+ is…
• we plan to fill SNO with liquid scintillator• we also plan to dope the scintillator with neodymium to conduct a
double beta decay experiment (first run is with Nd)• to do this we need to:
– install hold down ropes for the acrylic vessel– buy the liquid scintillator– build a liquid scintillator purification system– minor upgrades to the cover gas– minor upgrades to the DAQ/electronics– change the calibration system and sources
• SNO+ is fully funded with a major CFI and some advanced funding from NSERC
Sudbury Neutrino Observatory
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SNO+ Physics Program
• search for neutrinoless double beta decay• neutrino physics
– solar neutrinos– geo antineutrinos– reactor antineutrinos– supernova neutrinos
SNO+ Physics Goals
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SNO+ Liquid Scintillator
• “new” liquid scintillator developed– linear alkylbenzene (LAB)
• compatible with acrylic, undiluted• high light yield• pure (light attenuation length in excess of 20 m at 420 nm)• low cost• high flash point 130°C safe• low toxicity safe• smallest scattering of all scintillating solvents investigated• density r = 0.86 g/cm3
• metal-loading compatible– SNO+ light output (photoelectrons/MeV) will be approximately 3-4×
that of KamLAND• ~900 p.e./MeV for 54% PMT area coverage
58 Daya Bay and Hanohano plan to use LAB; others LENS, Double CHOOZ, LENA, NOnA considering
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Scintillator Purification
• prelim design completed by KMPS (engineering company that designed the Borexino scintillator purification)
• sizing completed, operating temperatures and pressures, flow rates calculated, performance simulated…
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Rope Configuration
• Analytic study of rope tensions and geometrical placement for PSUP penetrations
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