Upload
archer
View
34
Download
0
Embed Size (px)
DESCRIPTION
ニュートリノ物理 発展と動向. What do we know today? Solar Neutrino results (SK & SNO) First direct observation of oscillation in solar n Atmospheric neutrino results Atmospheric n deficiency : n m n t LSND and KARMEN More than 3 neutrinos? Present status of K2K What should be (shall be) done next - PowerPoint PPT Presentation
Citation preview
1
ニュートリノ物理発展と動向 2002年1月16日
@国際高等研究所京都大学大学院理学研究科
西川公一郎
1. What do we know today?
• Solar Neutrino results (SK & SNO)
– First direct observation of oscillation in solar
• Atmospheric neutrino results
– Atmospheric deficiency
• LSND and KARMEN
• More than 3 neutrinos?
• Present status of K2K
2. What should be (shall be) done next
3. Conclusion
2
3 Generations MNS matrix
• 3 angles and 1 phase
e2i
3
2
1
321
321
3e2e1ee
E2
m
UUU
UUU
UUU
2323
2323i
13i
13
1313
1212
1212
cossin0
sincos0
001
ecos0esin
010
sin0cos
100
0cossin
0sincos
U
propagation
23223
213
24212 eV10m)m()eV10(m
solar e : m2 <10-4eV2 no
reactor e : (Chooze, Pal-Verde) Ue3 ~ small
atm. m2 >10-3eV2 and
3
Measurements at m2>10-3eV2 (L/E ~ several 100 (km/GeV))
m223~m2
13>>m212
E
Lmsin2sincos
2232
232
134
E
Lmsin2sincos
2232
132
232
e
E
Lmsin2sin1
2232
132
ee
Three generation ?mixing anglemass difference
4
Solar neutrinoe =
1. Standard Solar Model (SSM) and experiments
2. New SNO results
3. Super-Kamiokande update to 1286 days
4. Summary of the status
5
Sources of Solar Neutrinos
http://www.sns.ias.edu/~jnb/
SNO
Each experiment is seeing different sources
Standard Solar Model relates different kinds of experiments
Target Data / SSM(BP2000)
・ Homestake 37Cl 0.32±0.03
・ Kamiokande e- (water) 0.54±0.07
・ SAGE 71Ga 0.58±0.06
・ GALLEX+GNO 71Ga 0.57±0.05
・ SK e- (water) 0.465±0.015
74 ±775 +8-7
GaH2O37Cl SuperK Kamioka SAGE GALLEX(+GNO)
0.47±0.020.54±0.07
Homestake
2.56 ±0.23
8.1 +1.4-1.1 SNU 129 +9
-7 SNU1.0
Theory7Be8B
pp, pepCNO
Experiments
+0.20-0.16
Be 0
B 0.5
then….no need of osc.
Solar Neutrino Experiments (as of 2000)
7
8
Measurement of 8B (SK and SNO)
• SK e + e e + e CC : NC =6:1 (1)– forward peaked
• SNO e + d e + p + p CC (2)
e + e e + e CC : NC =6:1•(1)-(2) NC event rate due to 8B
•should be constant for oscillation among active neutrinos
–8B Flux measurement with neutral current interaction
•Confirm SSM (Be, B pp chain = solar luminescence)
•Flux (deduced from NC) – Flux (deduced from CC)
= Non e components
•SSM independent evidence of oscillation
9
New SNO results• Teff=6.75 Mev
• No large spectrum distortion
• Charged current :
( Q=1.44MeV)
e + D p + p + e (CC)
• electron scattering :
+ e e + (ES)
12612.0
01.0scm10)07.075.1(
12616.0
14.0scm10)34.039.2(
10
SK
CC = e
ES = e +0.154 ,
SNO CC = 1.750.15SK ES = 2.320.09
, = 3.691.13
X = 5.440.99 (total active 8B neutrino flux)(SSM = 5.05+1.01/-0.81)
[x106/cm2/s]
SK + SNO combined
11
Super KamiokandeSuper Kamiokande
41.4m
39.3m
50kton stainless steel tank
Outer detector 1867 of 8” PMT
Inner detector11146 of 20” PMT
Ikeno-yamaKamioka, Gifu
Mozumi Atotsu
3km 2km
1km(2700mwe)
12
May 31, 1996 - Oct.6, 2000 1258 days
e-
sun
COSsun
Ee = 5.0 - 20 MeV
~18500 solar events
(14.7 events/day)
+0.016-0.013
8B flux : 2.32 0.03 [x 106 /cm2/sec] Data
SSM(BP2000) = 0.451 0.005
+0.08-0.07
(using Ortiz et al. spectrum shape(nucl-ex/0003006))
Direction to the Sun
13
e→()
99% C.L.
Oscillation parameters based on flux of Homestake, GALLEX, SAGE and SK
122
2
12212
122
m12
2
2sin2cosm
EV2
2sin2sin
VE2
m2cosV
21212
c
e
c
only e has e CC
14
Small Mixing angle solution
Seasonal effect, spectral distortion
P( e
→
e)
Large Mixing solution
Low
Just-so
solar neutrino spectrum
Day
Night
Spectral shape distortion
Day/night difference
oscillation in solar neutrino
Day/night in pp
Day/night, spectrum with higher precision
15
Earth density: =5g/cm2 (average),13(at core) Affect to oscillations for m2 = 10-6 - 10-4 eV2
(Night-Day)
(Night+Day)/2
e
1%2%
10%
80%
slight negative
Day/Night Effectregeneration through the earth
N-D = 0.033 0.022(stat.) (N+D)/2
0.0130.012 (sys.)
16
(6.310-3, 510-6eV2) SMA
(0.75, 6.310-11eV2) Justso
(0.8, 3.210-5eV2) LMA
Bad fit for SMA and Just-so solutions.
Spectrum shape comparison
uncertainties of absolute energy scale, energy resolution, 8B spectrum shape
17
Excluded by SK zenith angle spectrum at 95%C.L.Allowed by global fit (Cl + Ga + SK flux) at 95%C.L.
95%CL
m2(e
V2)
sin22
e e sterile
. e
2. LMA prefered
18Fogli et.al. hep-ph/0106247
19
2 for eccentricity: 3.9 / 7 d.o.f. (79% C.L.)
2 for flat: 8.1 / 7 d.o.f. (32% C.L.) )
Sunspot #
Time variation of the flux, seasonal
No magnetic field dep.No distance dep. (Just-so)
20
Kamioka Liquid scintillator Anti-Neutrino Detector
http://www.awa.tohoku.ac.jp/KamLANDKamLANDKamLAND
1000m3 liquid scintillator3000m3 oil+water shield1300 17-inch PMTs +600 20-inch PMTsAnti-e from reactors (L~170km)Detect e+ from e + p e+ + n (Eth = 1.8 MeV)
21
From K.Inoue (Tohoku Univ.)
KamLAND: sensitivityKamLAND: sensitivityWhat(3)
22
Conclusion on solar neutrinos
• There is non-electron neutrinos in solar neutrino oscillation!• SSM is OK within 20%• Just-so, LOW, and SMA are disfavored
– 93 % C.L. by SK zenith-spectrum analysis for e→ oscillations.
• Sterile is disfavored with 95% C.L. by zenith-spectrum.
• Energy spectrum is consistent with flat.
• day/night difference is 3.3±2.2 +1.3/-1.2 %.
• Large angle solution : testable in KAMLAND• Also by Borexino
23
Interaction in the rock
FC + PC
through-going muons
stopping muons
Initial neutrino energy spectrum
FC
Through-going muons
Stopping muons
Event topologyPC
24
Zenith angle distribution (Soudan 2)
cos log(L/E)
HiRes events (106.3±14.7 nm, 132.8±13.4 ne)
Decay excluded by 2
25
Zenith angle distribution
No oscillation
Δm2=2.5x10-3
sin22θ=1.0(best fit)
26
allowed region
FC + PC + up-through +up-stop +Multi-ring
χ2min=142.1/152dof
@(Δm2,sin22θ)=(2.5x10-3,1.0)
27
v.s. s
C.C. N.C. X ○s X X
•NC in the earth ( matter effect ) PC, up through μ(high energy) FC (low energy)
CC interaction in SK detector appearance
28
matter effect in the earthsin22θm =
sin22θ( -cos2θ)2+sin22θ2VEν
Δm2
sin22θ~ 1, Eν>20GeV sin22θm 1≪
PC, Evis>5GeV<Eν> ~ 25GeVup/down ratio
up through going μ<Eν>~ 100GeVvertical/horizontal ratio
νμ ー ντ
νμ ー νs
νμ ー νs
νμ ー ντ
29
v.s. s
high energy PC up/down ratio
up through μ vertical/horizontal ratio
NC enrigh multi ringevent up/down ratio
νμ ー νs
νμ ー ντ
νμ ー ντνμ ー ντ
νμ ー νs
νμ ー νsdata
30
ντ + N → τ + N’ +π+π..., e, +hadrons(,....)
appearance study
CC interaction
Many hadrons are produced.
Optimized by using onlydownward going events.
compare upward going data and MC.
enriched sample
νμ-ντ
with ντCC
νμ-ντ
w/o ντCC
# of obs. τ efficiency# of τ (eff. corrected)
43±1742%103±41
+8- 11
+18- 26
• ~ 2σ excess of τ-like events.• Data are consistent with νμ-ντ oscillation with ντCC.
31
Summary of atmospheric neutrino observation
• Oscillation parameters for : m2 = 1.6 ~ 3.6 x 10-3 eV2, sin22 > 0.90 (90%CL)
• Decay scenario is disfavored with > 2for dcy>>osc and dcy<<osc
s is strongly disfavored
• Excess from leptons: 1.5 ~ 2• Future
– Implement 3D flux calculations
– Study more on -lepton production
– Study on the mixed final state +s
32
LSND and KARMEN
Stopping onlydecayabsorbed in nuclei
componentno
,,
e
e
e+p→e++n n+A→A’+
33
LSND-Karmen-Nomad comparison
Small m2
region remains
34
35
mass - oscillationsallowed regions
LSND, if true, more than 3 neutrinos ?No sign in solar and atmospheric neutrino obs.
36
K2K( Testing atmospheric observation with accelerator neutrino beam)
• Distance and direction fixed
neutrino energy (E• Neutrino beam just after birth• 99% decay volume)
)E
Lm27.1(sin2sin.prob
222
L=250km
37
Bird’s Eye Neutrino Beam Line
38
Spectrum Distortion at Off axis(4 mrad) (MC)
1 06
1 07
1 08
1 09
0 1 2 3 4 5P (G e V /c )
O n a x i s f l u x
O f f a x i s f l u x
mradian accuracy is more than enough
39
stability monitor
200m1ch=5c
m =0.2
5 mrad.
<1mrad.
-1mrad.
+1mrad.
40
Near neutrino detector
Fine Grained Detector
300m from target
41
Neutrino Beam Direction (MRD profile)
Fitted centerx: 1±5cmy: - 10±4cmCentered within sys. err. of 20cm
SK direction(0.7mrad).
x, x
標的
near det.
300m
400cm
42
Stability of Spectrum
Muon Energy of MRD events
Muon Energy of 1kton events
43
K2K Results(June ‘99 – July ‘01)
1. Number of events• 1 kton water Chrenkov detector
SK almost counting experiment
– NC/CC, spectrum shape, interaction model
errors almost cancell
2. Spectrum distortion• non-QE , NC must be subtracted
44
SK EventsTspill TSK
GPS
No Decay-eHE Trig.Evis cut (30MeV)
No act. in OD(fully contained)
Exp’edAtm BG <10-3 in1.5s window
56 in fid. vol.
-0.2<TSK-TSpill-TOF<1.3sec
TOF~1msec
1sec
45
Dominant Systematic Errors •uncertainty of far-near ratio (~7%) and •uncertainty of 1kt fiducial volume (~4%).
46
Reconstructed E and muon directionFully contained 1-ring -like (22.5kt)
Need to estimate syst. err. Note: m2=310-3 eV2 corresponds to 600 MeV E
MC w/o osc.
47
Summary of K2K• Accumulated 4.5x1019POT @ SK from Jun ’99 to July
’01. (1.0 1020 protons in 2004)
• Neutrino beam is well under control Can extrapolate spectrum and flux from Near to Far
• # of fully contained events in fiducial volume @ SKObserved: 56, Expected with null oscillation 80
Probability of null oscillation < 3%
• Spectrum analysis, especially improving low energy region, just started– Pion production measurements @ CERN (HARP)– Upgrade in summer 2003
+7.3-8.0
48
• Atmospheric neutrinos– Where ( m2 =1.6·10-3 ~ 4·10-3 eV2 , sin22.– Most likely
• Solar neutrinos– LMA likely Large 12 ,m2
12 ~10-5 : CPV asym. can be large
• Reactor neutrinos– sin2213<0.1 for atmospheric m2 region
• K2K – Decrease over 250km of ~1GeV neutrino– Spectrum distortion
• Minos, MiniBooNE, CGN, Kamland– Oscillation pattern, appearance, LSND, LMA
• What is the best bet for the next step ?
49
Final goal (my own view)• Our own existence ?
– (near) GUTs scale physics• Mass-Interaction : mixing (or
?)• Small neutrino mass
– Existence of CP-violation in lepton sector (lepto-genesis)
– Baryon number non-conservation• Very massive detector
50
• CPV in Kaon system was discovered just below Adair’s measurement
• CP phase is large in K,B (Jarlskog factor is small)
• No theorist predicted large mixing 23
• No strict prediction on 13 , • 14 order of magnitude extrapolation for proton dec
ay prediction
• One order of magnitude improvements are worth the effort !
• Major discoveries may be around the corner
51
CP Violation in Lepton Sector (Why e)
=0 for appearance exp!
e
Current limit
E2
L)mm(sin)UUUUIm(2
E4
L)mm(sin)UUUURe(4P
2i
2j
ij
*jji
*i
2i
2j2*
jjiij
*i
52
CP Violation(difference of particle and anti-particle)
sinsin
2sin
E
Lm
PP
PPA
13
12212
CP
Solar 10-4~10-5 eV2 0.8 for LMA
Reactor experiments (CHOOZ)ex at atmospheric m2 region<0.16
remain to be discovered) : first step : second step
E
Lmsin2sincos
2232
132
232
e
53
Precision second generation experiment
CP violation measurementOscillation pattern , , m2
Sub-GeV Beam + Large water Cherenkov detector Beam control-ability and stability Event reconstruction (single e, ) Energy reconstruction Event selection (GPS timing)
Meaurements = (E) x Flux(E) x Detector responseSystematic studies of (anti-v) interactionsDetector response
Near/Far extrapolation
54
sin2213 from appearance experiment e + n e + p
sin2213
Background in Super-K (as of Oct 25, 2001)
SignalSignal + BG e e total
0.1 12.0 10.7 1.7 0.5 24.9 114.6 139.5
0.01 12.0 10.7 1.7 0.5 24.9 11.5 36.4
0.5 sin2213
m2
Off axis 2 deg, 5 years
Off axis 2 deg, 5 years
Wor
k in
pro
gres
s
55
Schematic drawing of Hyper-Kamiokande
1 Mton (fiducial) volume: Total Length 400m (8 compartments)
56
Sensitivity(3)
Chooz excluded@m31~3x10-3eV2
JHFSK cannot discover 13
IF BG sys 2%
sin2213=0.01sin>0.55 (33deg)
large sin2213
sin>0.25 (14deg)
Study in progress !
57
Artificial Neutrino Sources
• Conventional neutrino beams
• Neutrino factory – Very small backgrounds– Continuous Spectrum
N,
N,
e
e
,NP ee100
58
J.Wilkes’ TableExperiment
Property
SK K2K MINOS ICARUS OPERA JHF-Kam MONOLITH
-factory
CNGS
(m223)
±%
50 20 10 10 20 3.3 6 2
(sin22 23)
±%
5 5 5 5 ? 1 4 2
Osc peak X? ○* ○? X(○atm) ? ○ ○ ○
appear-
ance
○? X ○ ○ ○ X ○ ○
sin2213 >0.1 >0.01 0.03 0.015 ? 0.006 ? 1~3x10-3
(s/) 0.2 X 0.05? 0.05 ? 0.2? ~0.2 0.01
decay ○? ~X ○ X(○atm) ? ○ ○ ○
Sign of m2 X X X X X X X ○
CP violation X X X X X ○ X ○
On-going experiments
(www.phys.washington.edu./~wilkes/NNO/)
59
Solar Neutrinos8B NC is consistent with SSMNon-e neutrino in solar neutrino flux Sterile disfavoredCl, Ga, SK flux and 8B spectrum, Day/Night almost eliminate SMA, LOW solution
Spectrum , Day/Night , NC high precision measurementsLong baseline reactor exp. test LMA solution (Kamland)Solar neutrino at low energy (Borexino, Xmass….)
Atmospheric Neutrinos1.6x10-3 <m2 < 4x10-3eV2 sin22 > 0.89 (90%C.L.)s oscillation is disfavored with 99%C.L.-enrich data is consistent with t oscillation with CC.
Still Statistics limited
Conclusion-1
•
60
Conclusion-2
Accelerator experiments K2K 97% CL energy distortion in a few years, if m2>2x10-3eV2 KARMEN/NOMAD eliminate m2>eV2 region of LSND
Sterile? (Mini-BooNE) Direct confirmation of OPERA, ICARUS
Dip in disappearance ?m232 (JHFSK,MINOS)
e appearance ( JHFSK) CP violation in lepton sector (JHF-HyperK)
0Majorana neutrino!