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Transcript of Neutrinos: The Big Questions and How to Answer Them (and Others) Manfred Lindner Technical...
Neutrinos: The Big Questions and How to Answer Them (and Others)
Manfred LindnerTechnical University Munich
„Future Perspectives in High Energy Physics“Kyungpook National University Sept. 28-Oct. 1, 2005, Daegu, Korea
Manfred Lindner The 8th ICFA Seminar 2
Motivation: Physics Beyond the SM
gauge hierarchy problemmH
2 ~ 2
SUSY ~TeV
3 generations, fermion rep.many parameters (mi ,mixings)unification into GUTs
m=(mD)TMR-1mD
~GUT
+seesaw
gauge bosons
Higgs
quarksleptons
experimental facts:Dark Matter & Dark Energyneutrino massesbaryon asymetry m> 0
Manfred Lindner The 8th ICFA Seminar 3
New Physics: Neutrino Sources
Sun
Earth
Atmosphere
ReactorsCosmology
Accelerators
Astronomy: SupernovaeGRBsUHE ‘s
Manfred Lindner The 8th ICFA Seminar 4
Parameters for 3 Light Neutrinos
mass & mixing parameters: m1 , m221, |m2
31| , sign(m231)
diag(eiei
normal invertedhierarchical or degenerate
questions: Dirac or Majorana absolute mass scale: m1
mass ordering: sgn(m231)
how small is 13, 23 maximal? leptonic CP violation LSND sterile neutrino(s) L/E pattern of oscillations
e
Manfred Lindner The 8th ICFA Seminar 5
Four Methods of Mass Determination
• kinematical
• lepton number violation Majorana nature
• oscillations
• astrophysics & cosmology
Manfred Lindner The 8th ICFA Seminar 6
Kinematical Mass Determination
Future: KATRIN 0.25 eV ? c.f. comological boundsKATRIN 0.25 eV
Manfred Lindner The 8th ICFA Seminar 7
Heidelberg-Moscow experiment
< 0.35 eV ?
| |
free parameters: m1 , sign(m231) , CP-phases 2, 3
Neutrino-less Double -Decay
-
Majorana 02 decay
Manfred Lindner The 8th ICFA Seminar 8
| m
ee|
in e
V
Lightest neutrino (m1) in eV
Phase II:
Phase III:
m1small mee =const. ~ (mij2)1/2 sign(m2
31)m1 large mee ~ m1
cosmological bound on m1
HM-claim ‚tension‘Phase I:
new experiments: CUORICINO, GERDACUORE, Majorana, …aim: (m31
2)1/2 ~ 0.05eV
Cosmology: syst. errors X10?02 nuclear matrix elements?theory: LR, RPV-SUSY, ...
lepton number violation
Feruglio Strumia Vissani
Manfred Lindner The 8th ICFA Seminar 9
described by~ two independent
2x2 oscillationssurprise: large mixings!
Neutrino Oscillation Signals
m221 = (8.2+0.3) * 10-5 eV2
tan212 = 0.39 + 0.05m2
31 = (2.2+0.6) *10-3 eV2
tan223 = 1.0 + 0.3sin2213 < 0.16
solar
Reactors: KAMLAND
atmospheric
LSND? MiniBooNE
Beams: K2KMINOS
Manfred Lindner The 8th ICFA Seminar 10
L/E Dependence: Atmospheric Oscillations
decoherence
decay
oscillation „dip"
oscillation
L/E dependence smeared out!
Manfred Lindner The 8th ICFA Seminar 11
Result:• 3,4 for decay• 3,8 for de-coherence• m2=2.4 10-3eV2
long baseline exp.
Bad L/E resolution for:• horizontal events (dL/dcosis big!)• events with small energy
cuts in the E-cosplane
SK II datadecoherence decay oscillation
Manfred Lindner The 8th ICFA Seminar 12
Testing Solar L/E with KamLAND
rate plus shape oscillations at 99.999995% CL
Best fit: m2=7.9+0.6-0.5×10-5eV2
tan2=0.46
improved tests of L/E:
• Super Kamiokande• KamLAND• MINOS• …
Manfred Lindner The 8th ICFA Seminar 13
Solar Neutrinos: Learning About the Sun
Topics:- nuclear cross sections- solar dynamics - helio-seismology- variability- composition
Observables: - optical (total energy, surface dynamics, sun-spots, historical records, B, ...)- neutrinos (rates, spectrum, ...)
Manfred Lindner The 8th ICFA Seminar 14
Learning from Atmospheric Neutrinos
primary cosmic-ray interaction in the atmosphere
cascade of secondaries,K
decay of secondaries
ee
neutrinos from decays of other particles
Issues (in flux models):- primaries (...)- atmosphere- cross sections- B-fields- shower models- ...
Manfred Lindner The 8th ICFA Seminar 15
The Future of Oscillation Physics
long baseline experiments with neutrino beams reactor experiments with identical near & far detector
m2 and ij regions improved oscillation experiments controlled sources & detectors
Aims: improved precision of the leading 2x2 oscillations detection of generic 3-neutrino effects: 13, CP violation
=
S13 3 flavour effects S13
x Majorana-
CP-phases
matter effects
precision neutrino physics
Manfred Lindner The 8th ICFA Seminar 16
New Neutrino Beams
• conventional beams, superbeams MINOS, CNGS, T2K, NOA, T2H,…
• -beams pure e and e beams from radioactive decays; ~ 100
• neutrino factories clean neutrino beams from decay of stored ’s
-
correlations & degeneracies
Manfred Lindner The 8th ICFA Seminar 17
New Reactor Experiments
identical detectors many errors cancel
E=4MeV 2km 4km 40km 80km
no degeneraciesno correlationsno matter effects
Double Chooz KASKA Braidwood Angra, …
Manfred Lindner The 8th ICFA Seminar 18
13 Sensitivity in the Next Generation
NOvA
T2K
Compare:• 5 years each • 5% flux uncertainty
next generation long baseline experiments
coming long baseline experiments
1 reactor +2 detectors
NOA
Huber, ML, Rolinec, Schwetz, Winter
Manfred Lindner The 8th ICFA Seminar 19
Leptonic CP-Violationassume: sin2213= 0.1 , =/2 combine T2K+NOA+reactor
m2 > 0 m2 < 0 90%CL 3
bounds or measurements of leptonic CP-violation leptonic CP-violation in MR baryon asymetry via leptogenesis
Manfred Lindner The 8th ICFA Seminar 20
Sensitivity Versus Time
-beamsneutrino factory
protondriver?
Manfred Lindner The 8th ICFA Seminar 21
-Beam and / or NeutrinoFactory
• very powerful • interesting options• ...technological challenges
further R&D required
-beams: Store instable isotopes in accelerators pure e beams
-factory: Produce and store ‘s decay: pure e + beams_
neutrino factoryInternational
Scoping
Study
Manfred Lindner The 8th ICFA Seminar 22
Incremental Path to a NeutrinoFactory
Era ofsensitivity &
precision
ISS: establish that afaster approach is possible
Era ofsensitivity &
precision
Manfred Lindner The 8th ICFA Seminar 23
What is precison neutrino physicsgood for?
unique flavour information tests models / ideas about flavour history: elimination of SMA
Manfred Lindner The 8th ICFA Seminar 24
The Value of Precision for 13
for example: sin2213 < 0.01
physics question: why is 13 so small ?
numerical coincidence symmetry
precision!
• models for masses & mixings• input: Known masses & mixings distribution of 13 „predictions“
• 13 often close to experimental bounds motivates new experiments 13 controls 3-flavour effects like leptonic CP-violation
Manfred Lindner The 8th ICFA Seminar 25
Further Implications of Precision
Provides also measurements or tests of:
• MSW effect (coherent forward scattering and matter profiles)• cross sections• 3 neutrino unitarity sterile neutrinos with small mixings• neutrino decay (admixture…)• decoherence• NSI• MVN, ...
• special angles: 13= 0°, 23= 45°, ... discrete f. symmetries?• special relations: 12+ C = 45° ? quark-lepton relation?• quantum corrections renormalization group evolution
Precision allows to identify / exclude:
Manfred Lindner The 8th ICFA Seminar 26
The Interplay of Topics
mass spectrum, mixings, CP-phases, LVF, 02decay, ...
SM extensions
flavour symmetries Leptogenesis,supernovae, BBN,structure formation,UHE neutrinos, ...
renormalization group
-parameters extremely valuable long term: most precise flavour info
neutrino properties:masses, mixings,
CP-phases, ...
Manfred Lindner The 8th ICFA Seminar 27
Neutrinos & Cosmology
• Dark Matter ~ 25% & Dark Energy 70% • mass of all neutrinos: 0.001 < < 0.02• baryonic matter ~ 0.04
neutrinos affect:
- BBN, structure formation
- baryon asymmetry, ...
Manfred Lindner The 8th ICFA Seminar 28
Cosmology and Neutrino Mass• ‘s are hot dark matter smears structure formation on small scales
•WMAP+2dFGRS + Lymass bound: m< 0.7 ... 1.2 eV• degenerate neutrinos m < 0.4 eV future improvements: ~factor 5-10 ?• comparison with 02, LSND • will be directly tested by KATRIN
f=/matter
Tegmark
Manfred Lindner The 8th ICFA Seminar 29
Baryon Asymmetry & Neutrinos
anti-mattermatterparticle anti-particle
symmetry
baryon-
asymmetry
theory observation
measured baryon asymmetry:
Necessary: Sakharov conditions:• B-violating processes sphalerons• C- and CP-violation contained in model • departure from thermal equilibrium < H
natural explanation of baryon asymmetry by leptogenesis
• minimal leptogenesis works nicely• different interesting variants ... a talk by itself
Manfred Lindner The 8th ICFA Seminar 30
• Collaps of a typical star ~1057 ‘s• ~99% of the energy in ‘s• ‘s essential for explosion • 3d simulations do not explode (so far... 2d3d, convection? ... )
Supernova Neutrinos
MSW: SN & Earth
Very sensitive to finite 13 and sgn(m2)
Dighe, Smirnov
Manfred Lindner The 8th ICFA Seminar 31
2 possibilities:
Supernova
neutron star or black hole
Keeps cooling... abrupt end of emission
• impressive signal of a black hole in neutrino light • neutrino masses edge of -signal
Manfred Lindner The 8th ICFA Seminar 32
Supernovae & Gravitational Waves
gravitational wave emission quadrupol moment of the explosion
additional information about galactic SN global fits: optical + neutrinos + gravitational waves neutrino properties + SN explosion dynamics SN1987A: strongest constraints on large extra dimensions
Dimmelmeier, Font, Müller
Manfred Lindner The 8th ICFA Seminar 33
Neutrinos from Glactic Center
galactic
center
p n
+ 0 ´s
HE ´s @ HESS, EGRET
SN shock front acceleration flux from GC signal @ km3 detectors
HESS: TeV ‘s
Manfred Lindner The 8th ICFA Seminar 34
Geo Neutrinos as Probes of the Earth
Neutrino flowNeutrino flow
Heat flowHeat flow
- radiogenic part of terrestrial heat flow ~80 mW/m2 total: ~40 TW - test geochemical model of the Earth, the BBulk SSilicate EEarth- test unorthodox ideas of Earth’s interior (K @ core, giant reactor)
Manfred Lindner The 8th ICFA Seminar 35
Geo-Neutrino Observation at KamLAND
U+Th geo- candidates: 25+19-18
BSE model expectation: 19 Observed e candidates 152 eventsExpected total backgrounds 127±13
Reactor 13C(,n)16O
238U232Th
Accidental
Expected total backgrounds
Expected total
2nd reactor results
Geo-
Manfred Lindner The 8th ICFA Seminar 36
Conclusions
Neutrinos probe new physics in many ways!
Manfred Lindner The 8th ICFA Seminar 37
New Ideas: LENAIdea: ~30 kt underground liquid scintillator detector neutrino properties (solar, atmospheric, reactor, beams) solar neutrino spectroscopy supernova relic neutrino detection galactic supernova burst detection geo neutrino detection proton decay p K+ (favoured in SUSY models) - K invisible in water - better energy resolution - K and decay producs observable in scintillator - t > 3 * 1034y
K
nsecscintillator good resolution
water~SKbad resolution
modulation
Manfred Lindner The 8th ICFA Seminar 38
combined
New Ideas: R2D2 - Reactor Experiments• Symmetric reactors,detectors:
– R1, R2, D1, D2 - may be different
– L11=L22 and L12=L21
• Separate events from R1 and R2
– R1 and R2 on/off times
– Neutron displacement
• Simplest case: 1d line-upHigh statistics: precise statistical separation
N11, N21, N12, N22 self-calibration:
N11/N21=N22/N12
oscillation
stable against size, backgrounds, ... Improved sensitivity
Rr
NN
NN4
4
12*21
22*11
1,5cm
6cm
R1
at detector D1:
R2
Manfred Lindner The 8th ICFA Seminar 39
13 in the Coming LBL Generation