neutrinos louvain, february 2005 alan martin arguably the most fascinating of the elementary...
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Neutrinos
Louvain, February 2005Alan Martin
Arguably the most fascinating of the elementary particles.Certainly they take us beyond the Standard Model !
=E = mc2
SuperK, SNO(CC)
ChlorineGalliumSNO(NC)
SuperK, SNO(CC)
ChlorineGalliumSNO(NC)
Solar Neutrino Problem (circa 2000)
Experiment ReactionHomestake e+
37Cl 37Ar+eSAGE e+
71Ga 71Ge+eGallex + GNO e+
71Ga 71Ge+eKamiokande +Super-Kamiokande x+ex+e
GALLEX : Ga (e )SSM (e )
0.58 0.05
SAGE : Ga (e )
SSM (e )0.60 0.05
Homestake : Cl (e )
SSM (e )0.34 0.03
Super -K : SK (x )
SSM (e )0.451 0.015
0.017
eitherSolar models are incomplete/incorrect
orNeutrinos undergo flavor-changing
transformation
Sudbury Neutrino Observatory
1700 tonnes of inner shielding H2O
12.01m dia. acrylic vessel
17.8m dia. PMT Support Structure9456 20-cm dia. PMTs56% coverage
5300 tonnes of outer shielding H2O
Urylon liner
1006 tonnes D2O
Nucl. Inst. Meth. A449, 127 (2000)
2 km
to
su
rfac
e
Detecting at SNO
NCxx
npd
ES -- ee x x
CC-epd e p
• Low Statistics • (e) 6 () 6 ()
• Strong directionality:
• Measurement of e energy spectrum
• Weak directionality:
• Measure total 8B flux from the sun• e
1 0.340cos
e 18 (Te 10 MeV)
See : Phys.Rev.Lett. 89 (2002) 011301 Phys.Rev.Lett. 89 (2002) 011302
Solar Model predictions are verified: [in 106 cm-2 s-1]
Missing Solar ’s Found
e 1.76 0.05
0.05(stat.)0.09
0.09(syst.)106 cm 2s 1
3.410.45
0.45(stat.)0.48
0.45(syst.)106 cm 2s 1
8B shape constrained fit:
No 8B shape constraint:
CC ( e ) e
NC ( x ) e
ES ( x ) e 0.15
Null hypothesis of no flavour transformation rejected at 5.3
SSM (BP01) 5.05 1.01
0.81
SNOconstrained 5.09 0.44
0.43(stat.)
0.46
0.43(syst.)
SNOunconstrained 6.42 1.57
1.57(stat.)
0.55
0.58(syst.)
If CPT is conserved…(and LMA…)
Solar e
Predicts deficit in
Reactor e
~100 to 200 km
Complementary!
Why Kamioka?
P e sin2 2 sin2 1.27 m2
[eV2
] L[m]
E [MeV]
With L 175 km, E 5 MeV
Sensitive to m 2 2
5
175,000 1.27
4 10 5 eV2
51 reactors in Japan,80% of flux (or 68.5 GW of reactor power) from baseline of ~140 to 210 km
Is Oscillation Really the Solution?Kamioka Liquid scintillator Anti-Neutrino Detector (KamLAND)(Kamioka, Gifu Prefecture, Japan) reactor @ “right” baseline for directly testing the currently favoured LMA region
e p n e
e e 2
n p d (2.2 MeV)
2x coincidence
1 kt liquid scintillator as target
(inverse decay)
Reactor Anti-Neutrino FluxN
obs/N
no o
scill
atio
nNobserved – NBKG
Nno oscillation
= 0.611 ± 0.085 (stat) ± 0.041 (syst)
First observation of reactor anti-neutrino deficit
LMA prediction: m2 = 5.5x10-5 eV2
sin2 2 = 0.833
SuperK, SNO(CC)
ChlorineGalliumSNO(NC)
Electron neutrinos asexpected.
Evidence of mu-tauneutrino oscillations.
Should see evidenceof upgoing tau neutrinos
Atmosphericneutrinos
56 events seen---80 expected
0
4
2
8
10
6
-2
t
b
cs
d u
e
Log10m/eV
(m2atm)1/2
( m2sol)1/2
Upper limit on m
Neutrino masses are really special!
mt/(m2atm)1/2~1012
WMAP & LSS
KamLAND
Massless ’s?
• no R
• L conserved
Small masses?
• R very heavy
• L not conserved
/dm
dm
6p 4He + 2p +2e+ + 2
Twice
4p + e- 4He + e+ +2
Solar neutrino mixing
SuperK, SNO(CC)
ChlorineGalliumSNO(NC)