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Neutrinos as Probes of New Physics
Manfred LindnerTechnical University Munich
SUSY05The 13th International Conference on Supersymmetry and Unification of Fundamental Interactions July 18-23, 2005, IPPP Durham, UK
Manfred Lindner SUSY05 2
New Physics: Beyond the Standard Model
Two directions beyond SM:• EW symmetry breaking & hierarchy problem Higgs, SUSY, ... LHC, LC, ...• flavour problem origin of generations, flavour symmetries, q-l relations, .... neutrino physics, ...
Experimental facts• Cold Dark Matter & Dark Energy exist!• neutrino masses have been detected!• baryon asymetry of the universe m> 0
physics beyond the standard model
Manfred Lindner SUSY05 3
New Physics: Neutrino Sources
Sun
Earth
Atmosphere
ReactorsCosmology
Accelerators
Astronomy: SupernovaeGRBsUHE ‘s
Manfred Lindner SUSY05 4
Parameters for 3 light Neutrinos
diag(eiei
diag(eiei
4 different methods:
• kinematical
• lepton number violation Majorana
• oscillations
• astrophysics & cosmology
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Kinematical Mass Determination
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Heidelberg-Moscow experiment
< 0.35 eV ?
| |
free parameters: m1 , sign(m231) , CP-phases 2, 3
Neutrino-less double -Decay
-
Majorana 02 decay
Manfred Lindner SUSY05 7
| m
ee|
in e
V
Lightest neutrino (m1) in eV
Phase II:
Phase III:
m1small mee ~ (mij2)1/2
sign(m231)>0 ij=12
m1 large mee ~ m1
cosmological bound on m1
HM-claim ‚tension‘Phase I:
new exp. e.g. GERDAaim: (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 SUSY05 8
Neutrino Oscillation Signals
m2
21= 7.9 10-5 eV2
sin212 = 0.314m2
31= 2.4 10-3 eV2
sin223 = 0.44
solar
Reactors (KAMLAND)
atmospheric
LSND? MiniBooNE
Beams (K2K)
Manfred Lindner SUSY05 9
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 SUSY05 10
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- X-sections- B-fields- shower models- ...
Manfred Lindner SUSY05 11
The Future of Neutrino Oscillations
„long baseline“ experiments with neutrino beams and reactors
1) Improved precision of the leading 2x2 oscillations 2) Detection of generic 3-neutrino effects 13, CP-phase sgnm2
precision neutrino physics
3 flavour-oscillations
+ matter effects sgnm2
=
S13 3f-effects S13
x Majorana-
CP-phases
Manfred Lindner SUSY05 12
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 SUSY05 13
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 SUSY05 14
Long Term Ideas: -Beam & -Factory
• very powerful• interesting options• many good ideas• ...technological challenges
further R&D required
-beam idea: Store instable isotopes in accelerators pure e beams
-factory idea: Produce and store ‘s decay: pure e + beams
_
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What is precison neutrino physicsgood for?
unique flavour information tests models / ideas about flavour history: elimination of SMA
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13: What to expect from Flavour Models
For example: Ue3 in models with U(1) flavour symmetry Altarelli, Masina
[SS] [SS]
[SS] [NoSS]
Ue3 peaks close
to Chooz bound
sin2213<0.02 would select a very narrow subset of models
0.02 < sin2213 would not favour a particular model or spectrum
``anarchy’’= random numbers also favours 13 close to bounds
de Gouvêa, Murayama
Manfred Lindner SUSY05 17
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 CP-violation
Manfred Lindner SUSY05 18
Further Implications of Precision
Provides also tests of:
• MSW effect (coherent forward scattering and matter profiles)• 3 neutrino unitarity sterile neutrinos with small mixings• neutrino decay• 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 SUSY05 19
Mass Models & Renormalization
low energies:• small masses• large mixings
high energies:• mass models• flavour-symmetries• GUT-models, ...
renormalization group running
atmospheric
solar
reactor
bi-maximal
Small or even zero
MSSM example:Antusch, Kersten, ML, Ratz
23=
13 versus limit/value
Manfred Lindner SUSY05 20
Neutrino Mass Operators
d=4 renormalizable mass operatorsnatural scale symmetry
xL
xL
SM with L only m=0 introduce R = 1L
xx
L R
<> = v
R RgN
Majorana, L/
R
L
RD
DRL Mm
m
0
seesaw mechanism (type I)
m=mDMR-1mD
T mh=MR
For m3 ~ (m2atm)1/2, mD ~ leptons MR ~ 1011 - 1016GeV
neutrinos are Majorana particles , m probes ~ GUT scale physics! smallness of neutrino masses high scale of L, symmetries of mD , MR
/
Manfred Lindner SUSY05 21
More Mass Operators
xL L
<L>ML = 0 / m=ML - mDMR
-1mDT
Seesaw type II
More general:• mass matrix for all neutrino-like fields• every term has a natural scale symmetries GUT, flavour symmetry, lepton number, ...• diagonalization complicated dependence on all parameters
mechanisms to produced large mixings: e.g. sequential dominance King, ...
Manfred Lindner SUSY05 22
Screening
fit fermions into GUT representations relation between Yukawa couplings, e.g. E6
Assume: L, CR, S
double seesaw
complete screening of Dirac structure
m Planck scale symmetries, QLC, ... ML, Schmidt Smirnov
Manfred Lindner SUSY05 23
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 SUSY05 24
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 SUSY05 25
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 SUSY05 26
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 SUSY05 27
• 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
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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 SUSY05 29
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
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Neutrinos from Glactic Center
GC
p n
+ 0 ´s
HE ´s @ HESS, EGRET
flux from GC signal @ km3 detectors
HESS: TeV ‘s
Manfred Lindner SUSY05 32
• X-sections• NuTEV-anomaly• GRBs• AGNs• horizontal air showers @ Auger• regenerationOWL, ...• ...• theory: - models of -masses & mixings & RGE effects - scenarios with N>3 (sterile ‘s + small mixings) - limits on neutrino decay - bounds for non-standard interactions - big bang nucleosynthesis - conncetions to >SM & electro-weak symmetry breaking - GUTs, discrete flavour-symmetries - extra dimensions, strings, ... - ...
Other Topics (not covered)
Manfred Lindner SUSY05 33
Conclusions
Neutrinos probe new physics in many ways!