status and future of n -physics
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Status and Future of n -physics. What do I talk about?. Motivations Oscillations Status Open Questions Near Future Not so far Future Conclusions. Why are we doing ν -physics?. SM is very successful but it leaves a lot of questions open - PowerPoint PPT PresentationTRANSCRIPT
Hamburg 24.10.2005
Björn Wonsak
Status and Future of -physics
Hamburg 24.10.2005
Björn Wonsak
What do I talk about?
MotivationsOscillationsStatusOpen QuestionsNear FutureNot so far FutureConclusions
Hamburg 24.10.2005
Björn Wonsak
Why are we doing ν-physics?
SM is very successfulbut it leaves a lot of questions open
(e.g. astrophysical questions, like big bang, matter-antimatter asymmetry, supernovaes, etc.)
we want to understand physics beyond the SMThere are two ways to do that:
High Energies bigger accelerators
Study rare, tiny effects more statistics, lower background
Hamburg 24.10.2005
Björn Wonsak
Why are we doing ν-physics?
Tiny effect (m/E)2~(eV/GeV)2=10–18 !
Suitable methode: InterferometryNeeds coherent source
Needs Interference (i.e., large mixing angles)
Needs long baseline
All this is given us by nature:
Neutrino Interferometry (Oscillations) is a unique tool to study physics at very high scales !!!
Lowest order effect of physics at short distances !!!
Hamburg 24.10.2005
Björn Wonsak
What are ν-oscillations?
Flavour eigenstates e,, are not the mass eigenstates 1,2,3
neutrino mixing
3
2
1
321
321
321
UUUUUUUUU eeee
This leads to oscillations between the e,, like in the Kaon system
ν must have different masses (not all are massless) Leptonflavour is not strictly conserved
Already beyond the SM !
Pontecorvo-Maki-Nakagawa-Sakata (PMNS) Matrix:
Hamburg 24.10.2005
Björn Wonsak
What are ν-oscillations?
3
2
2323
2323
cssc
Flavor eigenstates , Mass eigenstates 2,3 with m2, m3
W
vμ
μ
source createsflavor-eigenstates
v2
v3
propagation determined bymass-eigenstates
23,2
23,23,2 mpE
slightly different frequencies→ phase difference changes
vτ
W
τ
p,n hadrons
detector seesflavor-eigenstates
Hamburg 24.10.2005
Björn Wonsak
What are ν-oscillations?
Oscillation probability
2
sin2sin 22 P
E
Lm
2
2with
Pro
babili
ty t
o fi
nd
vτ
Distance x in Losz
Losz, Δm2sin2(2
θ)
experiment needs statistics
experiment needs energy resolution
Hamburg 24.10.2005
Björn Wonsak
What are ν-oscillations?
100
0
0
0
010
0
0
0
001
1212
1212
1313
1313
2323
2323 cs
sc
ces
esc
cs
sci
i
PMNSU
ji
ijjjii
ji
ijjjiivv
E
LmUUUU
E
LmUUUUP
2sin)(2
4sin)(4
2**
22**
If neutrinos are Majorana particles: 2 additional Majorana-Phases (CPV): α1, α2
Three flavour mixing:
Zero for CPconservation
3 mixing angles and 1 CP-violating phase
Hamburg 24.10.2005
Björn Wonsak
L/E is crucial !
sin2(212)sin2(213)
Example for 3 flavour Oscillation probability !
m213
m212
Hamburg 24.10.2005
Björn Wonsak
What do we know?
Atmospheric neutrinos Super-Kamiokande
Atmosphärische Beschleuniger
9.02sin
105.0
6.04.2
232
23223
eVm
Hamburg 24.10.2005
Björn Wonsak
What do we know?
Solar neutrinos
07.0
1.040.0tan
105.0
6.09.7
122
25212
eVm
KamLAND
Reaktor-Solar-
SNO
,e
Mass effects in the sun dominate !
Hamburg 24.10.2005
Björn Wonsak
What are ν-oscillations?
100
0
0
0
010
0
0
0
001
1212
1212
1313
1313
2323
2323 cs
sc
ces
esc
cs
sci
i
PMNSU
ji
ijjjii
ji
ijjjiivv
E
LmUUUU
E
LmUUUUP
2sin)(2
4sin)(4
2**
22**
If neutrinos are Majorana particles: 2 additional Majorana-Phases (CPV): α1, α2
Three flavour mixing:
4/104523
6/103012 1313
100
031
013
2
1
0
010
0
110
110
001
2
1
1313
1313
ces
esc
i
i
PMNSU
2
3,
2
11212 cs
1
12
1
1212
1212
131212
cs
cs
sc
U PMNS
Very different m2 in different sectors
Solar and atmospheric oscillations can be regarded as independent
2 flavor discription is sufficient
3 mixing angles and 1 CP-violating phase
Hamburg 24.10.2005
Björn Wonsak
What do we want to know?
Dirac or Majorana ?Absolute mass scale ?How small is θ13 ?CP-violation ?Mass hierarchy ?Verify Ocsillations ? LSND ? Sterile neutrinos ? CPT-violation ?
0: claim by Klapdor-Kleingrothaus !
direct measurement: Katrin aims for m<0,2eV
Diappearance energyspectra, apperance
can be adressed by oscillation experiments
need specialised experiments
Hamburg 24.10.2005
Björn Wonsak
What comes next?
low E neutrinos (few GeV): disappearance experiment 4 x1020 pot/year 2500 CC/year compare Det1-Det2 response vs E in 2-6 years sensitivity to m2
atm
main goal: reduce the errors on m223 and sin2223 as needed for sin2213
measurement
NUMI
MINOS
Minos
735km
Magnetized steel/scintillator calorimeter
started this year
Hamburg 24.10.2005
Björn Wonsak
NC/CC ratio measured
contains four neutrino interactions
Hamburg 24.10.2005
Björn Wonsak
Hamburg 24.10.2005
Björn Wonsak
What comes next?
τ appearance experiment(search for 13)
Emulsion Cloud Chamber (ECC)
1,8 kton mass
En ≈ 17 GeV
start end 2006
Hamburg 24.10.2005
Björn Wonsak
µ spectrometer
8 m
Target Trackers
Pb/Em. target
Extract selected brick
Pb/Em. brick
8 cm Pb 1 mm
Basic “cell”
Emulsion
Electronic detectors select ν interacting brickµ ID, charge and p
Emulsion AnalysisVertex searchDecay searche/γ ID, kinematics
technic already used by Donut
discovery anno 2000
Hamburg 24.10.2005
Björn Wonsak
Hamburg 24.10.2005
Björn Wonsak
What comes next?
Double Chooz
100-200 m
12.7 m3
12.7 m3
Search for θ13:
Doppel-CHOOZ Reaktorneutrino experiment (France)
2 reaktors: 8.4GW Pth2 reaktors: 8.4GW Pth
100-200m
1 km
Double-Chooz sensitivity for (m2 = 2.0-2.5 10-3 eV2): sin2(213) < 0.025-0.03, 90% C.L.
first data taking beginning 2007
Hamburg 24.10.2005
Björn Wonsak
sin2(212)sin2(213)
m213
m212
Double-Chooz
Kamland
Hamburg 24.10.2005
Björn Wonsak
What comes next to next?
The first Super-Beam: off-axis T2K, from Tokai to SK
monitor (beam direction and intensity)
energy spectrum and intensity
Same spectrum as SK, BG measurement
start around 2009
Hamburg 24.10.2005
Björn Wonsak
30kt liquid Scintillator detectorNUMI beam with 6.5 x 1020 pot/yrWith a new Proton Driver, 25 x 1020 pot/yr Superbeam!Bunch time information used –physics comes back to surface
850km
16mrad off-axis
e/e
appearancestart about 2011
Hamburg 24.10.2005
Björn Wonsak
212
223
22
223121313
323121313
223
213
2
sin2sincos
sincos2sin2sincossin2sin
sin2sin2sincossin2sin
sin2sin2sin)(
CP
CP
eP
NOvA
T2K
122
134222
132 2sincossin2sin)(1 eeP
)4/(312
ELm 23121
2 / mm with
Neutrino superbeams
Neutrino superbeams
Hamburg 24.10.2005
Björn Wonsak
5 year onlyrun
for maximal atmospheric mixing
with m2≈2,5•10-3 eV2
Hamburg 24.10.2005
Björn Wonsak
What have we learned?
Smart way to reach high energy scales Already physics beyond the SMA lot of interesting open questionsFirst measurements were highly succesfull time for precision measurements
A new intertesting experiment every year fast growing knowledge