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

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 I n 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 2 JV2

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) ‏ K2K (250 Km) ‏ MINOS (735 Km) ‏... Super-K JV3

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

5. non-zero  1 3 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” A similar hint is found in some atm analyses. A weak preference also evidenced in the MINOS data in the  -> e appearance channel 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. What if nsi are present? JV5

6. Impact of FC NSI We expect a degeneracy between  13 and FC … 1,2 sigma positive nsi values shift LMA towards bigger  12 alleviating the tension with KamLAND, the same way as a non-zero  13 A. Palazzo and JV, arXiv:0909.1535 [hep-ph ] Notice that such couplings are not incompatible with existing bounds 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 JV6

7. Full 3 + FC-NSI analysis Full degeneracy between  13 and the NSI coupling 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] Solar + KamLAND JV7

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

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

10.  1 3 “ROADMAP” Huber, Lindner, Schwetz, Winter, 2009 talks of Bongrand, Link & Kim 10 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

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

12. SOLAR ROBUSTNESS wrt ASTRO CZ Miranda et al PRL93 (2004) 051304 & PRD70 (2004) 113002 Both strongly disfavored by KamLAND RZ Burgess et al JCAP0401 (2004) 007 Probe RZ mag-fields & RZ-density-noise helioseismology & magneto-gravity waves Burgess et al MNRAS.348 (2004) 609 FROM NEUTRINO PROPERTIES TO SOLAR PHYSICS JV12

13. bounds on transition mag-moment in a turbulent magnetic field model 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 FROM THEIR EFFECT ON THE NEUTRINO-ELECTRON SCATTERING CROSS SECTION Grimus et al, NPB648, 376 (2003) ‏ Borexino sensitivity JV13

14. NSI IN SNOVAE 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 atm sol JV14 Valle PLB199 (1987) 432 NSI-INDUCED FLAVOR CONVERSION NEAR CORE

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

16. EXPLAINING NEUTRINO PROPERTIES 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,... TBM ansatz Harrison–Perkins–Scott King Babu et al PLB552 (2003) 207 Hirsch et al PRD69 (2004) 093006 Antusch, Kersten, Lindner, Ratz, Schmidt, 2005 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 Hirsch et al, PLB679:454- 459,2009 DBD A4 flavor predictions PRD78:093007 (2008) ‏ PRL99 (2007) 151802 PRD79:016001,2009. PRD72, 091301 (2005) ‏ JV18

19. 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 STILL DO NOT UNDERSTAND FLAVOR - flavor models correlate LFV phenomena - if linked to unification, hard to reconcile L- & Q-mixings OSCILLATIONS MAINLY ROBUST but NEED NON-OSCILLATION TESTS: B&DBD, COSMO & ASTRO 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 A4 PRD78:093007 (2008) ‏ PRL 99 (2007) 151802 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. mu-e conversion in nuclei Deppisch, Kosmas & JV NPB752 (2006) 80 Heavy leptons@LHC mu->3e vs mu->e gamma LOW-SCALE SEESAW-3 Ibanez Morisi JV PRD80 (2009) 23

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