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Neutrinos: Big Questions and How to Answer Them

Explore the mysteries of neutrinos, from their masses to oscillation patterns and cosmological implications, discussed in the 8th ICFA Seminar. Learn about methods of mass determination and future perspectives in high-energy physics.

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Neutrinos: Big Questions and How to Answer Them

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  1. Neutrinos: The Big Questions and How to Answer Them (and Others) Manfred Lindner Technical University Munich „Future Perspectives in High Energy Physics“ Kyungpook National University Sept. 28-Oct. 1, 2005, Daegu, Korea

  2. SUSY ~TeV experimental facts: Dark Matter & Dark Energy neutrino masses baryon asymetrymn> 0 gauge hierarchy problem dmH2 ~ L2 3 generations, fermion rep.many parameters (mi ,mixings)unification into GUTs mn=(mD)TMR-1mD ~LGUT +seesaw Motivation: Physics Beyond the SM gauge bosons Higgs quarks leptons The 8th ICFA Seminar

  3. Sun Astronomy:  Supernovae GRBs UHE n‘s Cosmology Reactors Atmosphere Accelerators Earth New Physics: Neutrino Sources The 8th ICFA Seminar

  4. diag(eia, eib,1) Parameters for 3 Light Neutrinos mass & mixing parameters: m1 , Dm221, |Dm231| , sign(Dm231) ne nm nt questions: Dirac or Majorana absolute mass scale: m1 mass ordering: sgn(Dm231)  how small is q13, q23 maximal?  leptonic CP violation LSND  sterile neutrino(s) L/E pattern of oscillations normal invertedhierarchical or degenerate The 8th ICFA Seminar

  5. Four Methods of Mass Determination • kinematical • lepton number violation  Majorana nature • oscillations • astrophysics & cosmology The 8th ICFA Seminar

  6. Future: KATRIN  0.25 eV  ?  c.f. comological bounds KATRIN  0.25 eV Kinematical Mass Determination The 8th ICFA Seminar

  7. - < 0.35 eV ? n Heidelberg-Moscow experiment | |  free parameters: m1 , sign(Dm231) , CP-phases F2, F3 Neutrino-less Double b-Decay Majorana n 0n2b decay The 8th ICFA Seminar

  8. cosmological bound on m1 HM-claim  ‚tension‘ new experiments: CUORICINO, GERDACUORE, Majorana, … aim: (Dm312)1/2~ 0.05eV | mee| in eV Phase I: Lightest neutrino (m1) in eV Phase II: Phase III: m1small  mee =const. ~ (Dmij2)1/2  sign(Dm231) m1 large  mee ~ m1 Feruglio Strumia Vissani Cosmology: syst. errors  X10? 0n2b - nuclear matrix elements? theory: LR, RPV-SUSY, ...  lepton number violation The 8th ICFA Seminar

  9. described by ~ two independent 2x2 oscillations surprise: large mixings! Neutrino Oscillation Signals solar Reactors: KAMLAND Beams: K2KMINOS atmospheric Dm221 = (8.2+0.3) * 10-5 eV2 tan2q12 = 0.39 + 0.05 Dm231 = (2.2+0.6) *10-3 eV2 tan2q23 = 1.0 + 0.3 sin22q13 < 0.16 LSND?  MiniBooNE The 8th ICFA Seminar

  10. oscillation „dip" L/E Dependence: Atmospheric Oscillations oscillation decay decoherence L/E dependence smeared out! The 8th ICFA Seminar

  11. Bad L/E resolution for: • horizontal events (dL/dcosq is big!) • events with small energy • cuts in the E-cosq plane SK II data decay decoherence oscillation • Result: • 3,4s for decay • 3,8s for de-coherence • Dm2=2.4 10-3eV2 • long baseline exp. 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 • … The 8th ICFA Seminar

  13. Solar Neutrinos: Learning About the Sun • Observables: • optical (total energy, surface dynamics, sun-spots, historical records, B, ...) • neutrinos(rates, spectrum, ...) • Topics: • nuclear cross sections • solar dynamics • helio-seismology • variability • composition The 8th ICFA Seminar

  14. Learning from Atmospheric Neutrinos • Issues (in flux models): • - primaries (...) • - atmosphere • - cross sections • B-fields • shower models • ... primary cosmic-ray interaction in the atmosphere cascade of secondaries p,K decay of secondaries m m nm nm ne nm ne nm neutrinos from decays of other particles The 8th ICFA Seminar

  15. x Majorana- CP-phases matter effects = q23 S13 3 flavour effects q12  S13  d The Future of Oscillation Physics • Dm2 and qij regions improved oscillation experiments • controlled sources & detectors • long baseline experiments with neutrino beams • reactor experiments with identical near & far detector Aims: improved precision of the leading 2x2 oscillations  detection of generic 3-neutrino effects: q13, CP violation  precision neutrino physics The 8th ICFA Seminar

  16. correlations & degeneracies New Neutrino Beams • conventional beams, superbeams MINOS, CNGS, T2K, NOnA, T2H,… • b-beams pure ne and ne beams from radioactive decays; g ~ 100 • neutrino factories clean neutrino beams from decay of stored m’s - The 8th ICFA Seminar

  17. New Reactor Experiments identical detectors  many errors cancel • Double Chooz • KASKA • Braidwood • Angra, … no degeneracies no correlations no matter effects E=4MeV  2km 4km 40km 80km The 8th ICFA Seminar

  18. coming long baseline experiments 1 reactor +2 detectors NOvA next generation long baseline experiments T2K • Compare: • 5 years each • 5% flux uncertainty NOnA q13 Sensitivity in the Next Generation Huber, ML, Rolinec, Schwetz, Winter The 8th ICFA Seminar

  19. Dm2 > 0 Dm2 < 0 90%CL 3s Leptonic CP-Violation assume: sin22q13= 0.1 , d=p/2  combine T2K+NOnA+reactor • bounds or measurements of leptonic CP-violation • leptonic CP-violation in MR baryon asymetry via leptogenesis The 8th ICFA Seminar

  20. Sensitivity Versus Time b-beams neutrino factory proton driver? The 8th ICFA Seminar

  21. b-beams: Store instable isotopes in accelerators  pure ne beams n-factory: Produce and store m‘s  decay: pure ne + nmbeams _ b-Beam and / or NeutrinoFactory • very powerful • interesting options • ...technological challenges • further R&D required neutrino factory International Scoping Study The 8th ICFA Seminar

  22. ISS: establish that a faster approach is possible Era of sensitivity & precision Incremental Path to a NeutrinoFactory Era of sensitivity & precision The 8th ICFA Seminar

  23. What is precison neutrino physics good for? • unique flavour information • tests models / ideas about flavour • history: elimination of SMA The 8th ICFA Seminar

  24. The Value of Precision for q13 • models for masses & mixings • input: Known masses & mixings •  distribution of q13 „predictions“ • q13 often close to experimental bounds •  motivates new experiments •  q13 controls 3-flavour effects • like leptonic CP-violation for example: sin22q13 < 0.01  • physics question: why is q13 so small ? • numerical coincidence • symmetry precision! The 8th ICFA Seminar

  25. Precision allows to identify / exclude: • special angles: q13= 0°, q23= 45°, ... discrete f. symmetries? • special relations: q12+ qC = 45° ? quark-lepton relation? • quantum corrections  renormalization group evolution 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, ... Further Implications of Precision The 8th ICFA Seminar

  26. The Interplay of Topics flavour symmetries Leptogenesis, supernovae, BBN, structure formation, UHE neutrinos, ... SM extensions neutrino properties: masses, mixings, CP-phases, ... renormalization group mass spectrum, mixings, CP-phases, LVF, 0n2b-decay, ... n-parameters extremely valuable  long term: most precise flavour info The 8th ICFA Seminar

  27. Neutrinos & Cosmology • Dark Matter ~ 25% & Dark Energy 70% • mass of all neutrinos: 0.001 <Wn< 0.02 • baryonic matter WB ~ 0.04 • neutrinos affect: • BBN, structure formation • baryon asymmetry, ... The 8th ICFA Seminar

  28. Tegmark fn=Wn/Wmatter Cosmology and Neutrino Mass • n‘s are hot dark matter  smears structure formation on small scales • WMAP+2dFGRS + Lya •  mass bound: Smn< 0.7 ... 1.2 eV • 3 degenerate neutrinos •  mn < 0.4 eV future improvements: ~factor 5-10 ? • comparison with 0n2b, LSND • will be directly tested by KATRIN The 8th ICFA Seminar

  29. theory observation  symmetry  baryon- asymmetry anti-particle particle matter anti-matter measured baryon asymmetry: natural explanation of baryon asymmetry by leptogenesis Baryon Asymmetry & Neutrinos • Necessary: Sakharov conditions: • B-violating processes  sphalerons • C- and CP-violation  contained in model • departure from thermal equilibrium  G < H • minimal leptogenesis works nicely • different interesting variants ... a talk by itself The 8th ICFA Seminar

  30. Supernova Neutrinos • Collaps of a typical star  ~1057n‘s • ~99% of the energy in n‘s • n‘s essential for explosion • 3d simulations do not explode • (so far... 2d3d, convection? ... ) Dighe, Smirnov MSW: SN & Earth Very sensitive to finite q13 and sgn(Dm2) The 8th ICFA Seminar

  31. 2 possibilities: • Supernova • neutron star or black hole • Keeps cooling... abrupt end of • n-emission • impressive signal of a black hole in neutrino light • neutrino masses  edge of n-signal The 8th ICFA Seminar

  32. Supernovae & Gravitational Waves gravitational wave emission  quadrupol moment of the explosion Dimmelmeier, Font, Müller • additional information about galactic SN • global fits: optical + neutrinos + gravitational waves • neutrino properties + SN explosion dynamics • SN1987A: strongest constraints on large extra dimensions The 8th ICFA Seminar

  33. HESS: TeV g‘s Neutrinos from Glactic Center n galactic center p HE g´s @ HESS, EGRET p+p0 HE n´s - SN shock front acceleration - n flux from GC  n signal @ km3 detectors The 8th ICFA Seminar

  34. Heat flow Neutrino flow Geo Neutrinos as Probes of the Earth • radiogenic part of terrestrial heat flow ~80 mW/m2 total: ~40 TW- test geochemical model of the Earth, the Bulk Silicate Earth- test unorthodox ideas of Earth’s interior (K @ core, giant reactor) The 8th ICFA Seminar

  35. Geo- 2nd reactor results Expected total Expected total backgrounds Reactor  13C(,n)16O 238U 232Th Accidental Geo-Neutrino Observation at KamLAND U+Th geo-n candidates: 25+19-18 BSE model expectation: 19 Observed e candidates 152 events Expected total backgrounds 127±13 The 8th ICFA Seminar

  36. Conclusions Neutrinos probe new physics in many ways! The 8th ICFA Seminar

  37. scintillator  good resolution water~SKbad resolution m K modulation nsec New Ideas: LENA • Idea: ~30 kt undergroundliquid 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+n (favoured in SUSY models) - K invisible in water - better energy resolution - K and decay producs observable in scintillator - t > 3 * 1034y The 8th ICFA Seminar

  38. High statistics: •  precise statistical separation •  N11, N21, N12, N22 • self-calibration: N11/N21=N22/N12 •  oscillation • stable against size, backgrounds, ... • Improved sensitivity at detector D1: combined 6cm R2 1,5cm R1 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-up The 8th ICFA Seminar

  39. q13 in the Coming LBL Generation The 8th ICFA Seminar

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