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Status of the Neutrino Physics

Status of the Neutrino Physics. Carlos Peña Garay IFIC, Valencia. Act 1 : Lepton mixing matrix and neutrino masses Discovery of neutrino oscillations induced by neutrino mass and determination of neutrino parameters. Solar & KamLAND flavor conversion. β = l osc / l matt.

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Status of the Neutrino Physics

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  1. Status of the Neutrino Physics Carlos Peña Garay IFIC, Valencia HQ&L 2010, Frascati

  2. Act 1 : Lepton mixing matrix and neutrino masses Discovery of neutrino oscillations induced by neutrino mass and determination of neutrino parameters

  3. Solar & KamLAND flavor conversion β = losc / lmatt Oscillations in vacuum and flavor conversion by matter index of refraction

  4. Solar and Reactor Neutrinos Solar neutrinos: stronger constraint on q12 KamLAND: stronger constraint on Dm221 Different sensitivity to q13 Lisi et al (2008) Gonzalez-Garcia et al (2010)

  5. Atmospheric and Accelerator Neutrinos Oscillations in vacuum and matter effects if nonzero q13 Atmospheric neutrinos: stronger constraint on q23 Accelerator neutrinos: stronger constraint on Dm231

  6. SK & Minos appearance Sensitivity to q13 in appearance Gonzalez-Garcia et al (2010)

  7. Status of q13 2011: Accelerator (T2K) & Reactor (D-CHOOZ, Daya Bay)

  8. Summary of neutrino parameters Gonzalez-Garcia et al (2010) Different pattern (>15s) for leptons and quarks: Sign of different origin

  9. Three-act play Act 2: Searches for unknown parameters Remaining job to complete the picture emerged by neutrino oscillations

  10. q13 and dCP Gonzalez-Garcia et al (2010) Weak sensitivity to CP phase 2011: Accelerator (T2K) Proposals studied: Superbeams, Betabeams, NuFact

  11. Mass splitting hierarchy Determine neutrino mass hierarchy (IH vs NH): - Very important for neutrinoless double beta decay - Depends on the magnitude of matter effects, and a nonzero q13 - No sensitivity in cosmological data: degeneracy

  12. Neutrino mass scale: Beta Decay Act 2: Searches

  13. Neutrino mass scale: Cosmology Sensitivity to the neutrino masses (matter-radiation eq. and growth of structures) Extra handle with sensitivity to the atmospheric splitting Jimenez et al (2010)

  14. Majorana mass: Majorana phases only relevant in processes involving Lepton Number Violation (na - nb) Helicity suppressed by smallness of neutrino masses

  15. From Osc. Data : me |<mnee>| = (T1/2 FN )1/2 FN = G0n |M0nf – (gA/ gV)2 M0nGT |2 |<mnee>| = |Smj Uej2 | = |Smj |Uej |2 eif|

  16. Three-act play Act 3: Some Open Problems/Opportunities Is there anything more? Are we ready for more surprises?

  17. LSND/Miniboone antineutrinos Excess (21+-14) in antinu appearance (0.5% chance of bckg.-only hypothesis) at the same L/E as in LSND, not seen in neutrino appearence Miniboone coll. (2010)

  18. Tests of amplitude of matter effects SNO (2010) Borexino (2010) Loose upper bound. Improved by 3s upturn, pep and 7Be neutrinos and 2s daynight Probe matter potential for different matter compositions: Sun (dominantly protons) and Earth (even protons, neutrons) Minakata et al (2010)

  19. Supernova neutrinos Dasgupta et al 2009 Collective oscillations due to neutrino-neutrino coupling might be relevant in supernova neutrinos

  20. Solar composition problem: Low Z/X Attemps to solve the discrepancy: Increase opacity below CZ? Increase Ne abundance? Enhance diffusion?

  21. How to extract core metallicities Haxton & Serenelli 2008, Haxton et al, 2010 Measured at the center of the Sun by Borexino and SK/SNO

  22. Conclusions Neutrino experiments have been very successful in measuring mixings and mass squared differences by neutrino oscillations of solar , reactor, atmospheric and accelerator neutrinos. Lepton and quark mixing matrices show a different pattern, suggesting a different origin of the masses. Present data still insensitive to mass splitting hierarchy, mass scale, small mixing angle and CP phase. Open problems offer an opportunity to test our fundamental description of the nature of neutrinos and understand physics at the neutrino sources.

  23. Conclusions Neutrino experiments have been very successful in measuring mixings and mass squared differences by neutrino oscillations of solar , reactor, atmospheric and accelerator neutrinos. Lepton and quark mixing matrices show a different pattern (>15s), suggesting a different origin of the neutrino and quark masses. More precision on the known mixings will constrain complementarity. Present neutrino data still insensitive to small mixing angle, CP phase, mass splitting hierarchy, mass scale and type. Depending on the small mixing, some parameters are within reach in running experiments. Is that all folks? We have little theoretical guidance but some open problems and tests of physics at sources

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