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OSCILLATION PARAMETERS CP VIOLATION & NSI J W F Valle IFIC/CSIC – U Valencia http://ahep.uv.es. http://ahep.uv.es. JV 1. 1. THE LEPTON MIXING MATRIX. Schechter & JV PRD22 (1980) 2227, PRD23 (1981) 1666 & PDG.

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  1. OSCILLATION PARAMETERS CP VIOLATION & NSI J W F Valle IFIC/CSIC – U Valencia http://ahep.uv.es http://ahep.uv.es JV1 1

  2. THE LEPTON MIXING MATRIX Schechter & JV PRD22 (1980) 2227, PRD23 (1981) 1666 & PDG • Even in its simplest unitary form K differs from quark mixing matrix, with two extra (Majorana) phases • In seesaw-schemes K is not unitary => extra angles and phases => new physics: new effects in neutrino propagation & charged LFV • To describe current oscill data we assume K real unitary JV2 2

  3. 1223 13 (before SNO'S LETA analysis) Schwetz et al, NJP 10 (2008) 113 [rev. Maltoni et al, NJP 6 (2004) 122] Homestake, SAGE+ GALLEX/GNO, Super-K, SNO Borexino KamLAND (180 Km)‏ ... Super-K K2K (250 Km)‏ MINOS (735 Km)‏ JV3

  4. ZOOMSchwetz et al, NJP 10 (2008) 113 c.f. e.g. Fogli et al, 2008 Lisi's talk JV4

  5. non-zero 13 vs FC-NSI in the solar neutrino sector Existing analyses show a weak preference (1.2-1.5 sigma) for non-zero 13 in the (Solar + KamLAND) analysis. Comes from sol-KL “clash” Though very weak note that solar transitions are dominated by matter effects, while the oscillations seen in KamLAND occur in the earth crust, where matter effects are negligible . A similar hint is found in some atm analyses. A weak preference also evidenced in the MINOS data in the -> e appearance channel What if nsi are present? JV5

  6. Impact of FC NSI A. Palazzo and JV, arXiv:0909.1535 [hep-ph] positive nsi values shift LMA towards bigger 12 alleviating the tension with KamLAND, the same way as a non-zero 13 We expect a degeneracy between 13 and FC … 1,2 sigma Davidson et al JHEP (2003) 0303:011 Barranco, et al , D73 (2006) 113001, D77 (2008) 093014 Abada, Biggio Bonnet, Gavela, Hambye PRD78 Esteban Huber JV PLB668:197201,2008 Gavela, Hernandez, Ota, Winter, PRD79 Malinsky et el, arXiv:0905.2889 [hep-ph] Bolanos et al PRD79 (2009) 113012 Notice that such couplings are not incompatible with existing bounds JV6

  7. Full 3 + FC-NSI analysis Full degeneracy between 13 and the NSI coupling Solar + KamLAND Tension between solar & KamLAND gets diluted among the two parameters FC NSI constitute a source of confusion which can mimic the preference for 13>0 1, 2 sigma A. Palazzo and JV, arXiv:0909.1535 [hep-ph] JV7

  8. ROBUSTNESS wrt NU-NSI Escrihuela et al, arXiv:0907.2630 Miranda, et al JHEP 0610:008,2006. 8 JV8

  9. RESOLVING Escrihuela et al, arXiv:0907.2630 Miranda, et al JHEP 0610:008,2006. Lowered threshold HE experiments useful SNO (LETA)‏ SK-III Borexino JV9

  10. 13 “ROADMAP” Huber, Lindner, Schwetz, Winter, 2009 talks of Bongrand, Link & Kim Note that a confusion between flavor-changing FC-NSI and 13 will pose a problem for parameter reconstruction in a future NuFact Huber, Schwetz, JV Phys.Rev.Lett.88:101804,2002. Phys.Rev.D66:013006,2002. JV10 10

  11. CPV IN NU-OSCILLATIONS aymmetries at % level maximal CPV Hirsch et al PRL99(2007)151802 From Nunokawa et al Prog.Part.Nuc.Phys. 60 (2008) 338 ISS report, S. King et al, Rep. Prog. Phys. 72 (2009) 106201 JV11

  12. SOLAR ROBUSTNESS wrt ASTRO RZBurgess et al JCAP0401 (2004) 007 CZMiranda et alPRL93 (2004) 051304 & PRD70 (2004) 113002 Both strongly disfavored by KamLAND FROM NEUTRINO PROPERTIES TOSOLAR PHYSICS JV12 Probe RZ mag-fields & RZ-density-noise helioseismology & magneto-gravity waves Burgess et al MNRAS.348 (2004) 609

  13. PROBING TRANSITION MAGNETIC MOMENTS Miranda et al PRL93 (2004) 051304 KamLAND anti-nu-e flux limit => SFP must be subdominant w.r.t. LMA oscillations bounds on transition mag-moment in a turbulent magnetic field model FROM THEIR EFFECT ON THE NEUTRINO-ELECTRON SCATTERING CROSS SECTION Grimus et al, NPB648, 376 (2003)‏ Borexino sensitivity JV13

  14. NSI IN SNOVAE atm sol NSI-INDUCED FLAVOR CONVERSION NEAR CORE Valle PLB199 (1987) 432 Interplay between SN physics & neutrino properties NU-NSI versus collective effects Raffelt's talk Esteban-Pretel et al PRD76 (2007) 053001 & arXiv:0909.2196 Nunokawa et al PRD54 (1996) 4356 JV14

  15. THE BIG QUESTIONS Singlet or 3plet fermion Type-I & III Minkowski 77 Gellman Ramond Slansky 80 Glashow, Yanagida 79 Mohapatra Senjanovic 80 Schechter-Valle, 80 Lazarides Shafi Weterrich 81 Foot et al 89 Triplet type-II Schechter-Valle 80/82 scale mechanism LOW-SCALE SEESAW Inverse seesawMohapatra-JV PRD34 (1986) 1642 Linear SeesawMalinsky et al PRL95 (2005) 161801 Inverse type-III Ibanez et al PRD 80 (2009) 053015 flavor structure JV15

  16. EXPLAINING NEUTRINO PROPERTIES Babu et al PLB552 (2003) 207Hirsch et al PRD69 (2004) 093006 TBM ansatzHarrison–Perkins–Scott King Antusch, Kersten, Lindner, Ratz, Schmidt, 2005 Many models Altarelli, Feruglio, Merlo Babu et al, Barr et al Frampton et al, Grimus, Lavoura Hirsch et al .. King et al, Ross et al Ma, Mohapatra et al, Plentinger & Rodejohan, Tanimoto, Raby et al, Ross et al, Zhang, ... JV16

  17. Seesaw scale may be low even within unification JV17

  18. ABSOLUTE NEUTRINO MASS -DBD Schonert - beta decay Katrin Drexlin - cosmology CMB LSS ... Pastor DBD A4 flavor predictions PRD78:093007 (2008)‏ PRL99 (2007) 151802 PRD79:016001,2009. PRD72, 091301 (2005)‏ Hirsch et al, PLB679:454-459,2009 JV18

  19. OSCILLATIONS MAINLY ROBUST but NEED NON-OSCILLATION TESTS: B&DBD, COSMO & ASTRO STILL DO NOT UNDERSTAND FLAVOR-flavor models correlate LFV phenomena - if linked to unification, hard to reconcile L- & Q-mixings PROBE HIGH FROM LOW SCALE 0RIGIN OF NEUTRINO MASS - via NSI strength novel neutrino propagation effects beyond oscillations + LFV effects in charged sector & new states at LHC SK-atmospheric and MINOS (appearance) data analysis may help to break degeneracy between 13 and FC NSI. Future reactors (Double-CHOOZ, Daya-Bay, RENO) will give a “clean” measure of 13, unaffected by NSI effects. non-confirmation of current 13 hints + persisting tension between solar and KamLAND would pose a new problem in the “solar sector” which might require NSI or other possible unaccounted effects JV19

  20. MERCI next slides are backup 20

  21. DBD & FLAVOR PRL 99 (2007) 151802 PRD78:093007 (2008)‏ A4 PRD72, 091301 (2005)‏ 21

  22. apart from NSI ... LFV & LHC effects INVERSE SEESAW-type1 Mohapatra-Valle, PRD34 (1986) 1642 INVERSE SEESAW-type3 Ibanez Morisi JV, PRD 80 (2009) 053015 LINEAR SEESAW Malinsky et al PRL95 (2005) 161801 LFV from NHL M=0.2-1TeV Hirsch, et al PLB679:454,2009 • natural ... t'Hooft • dynamical origin ... Bazzocchi, et al arXiv:0907.1262 [hep-ph] • LFV & CPV survive in massless neutrino limit, hence unsuppressed by small m-nu 22

  23. LOW-SCALE SEESAW-3Ibanez Morisi JV PRD80 (2009) mu->3e vs mu->e gamma mu-e conversion in nuclei Deppisch, Kosmas & JV NPB752 (2006) 80 23 Heavy leptons@LHC

  24. HIGH-SCALE SEESAW SUSY LFV DECAYS@LHC Hirsch et al PRD 78 (2008) 013006, Esteves et al JHEP05 (2009) 3 24

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