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Neutrinos: The Big Questions and How to Answer Them (and Others)

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. SUSY ~TeV. experimental facts: Dark Matter & Dark Energy

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Neutrinos: The Big Questions and How to Answer Them (and Others)

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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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