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OSCILLATION PARAMETERS CP VIOLATION & NSI
J W F ValleIFIC/CSIC – U Valencia
http://ahep.uv.es
JV1
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
2JV2
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
c.f. e.g. Fogli et al, 2008Lisi's talk
ZOOM Schwetz et al, NJP 10 (2008) 113
JV4
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”
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
Impact of FC NSI
We expect a degeneracybetween 13 and FC …
1,2 sigma
positive nsi values shift LMA towards bigger 12
alleviating the tensionwith 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) 0303:011Barranco, et al , D73 (2006) 113001, D77 (2008) 093014Abada, Biggio Bonnet, Gavela, Hambye PRD78Esteban Huber JV PLB668:197201,2008Gavela, Hernandez, Ota, Winter, PRD79Malinsky et el, arXiv:0905.2889 [hep-ph] Bolanos et al PRD79 (2009) 113012
JV6
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 sourceof confusion which can mimic
the preference for 13>0
1, 2 sigma
A. Palazzo and JV, arXiv:0909.1535 [hep-ph]
Solar + KamLAND
JV7
ROBUSTNESS wrt NU-NSI Escrihuela et al, arXiv:0907.2630 Miranda, et al JHEP 0610:008,2006.
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JV8
Escrihuela et al, arXiv:0907.2630Miranda, et al JHEP 0610:008,2006.RESOLVING
Lowered threshold HE experimentsuseful SNO (LETA)SK-III Borexino
JV9
13 “ROADMAP”Huber, Lindner, Schwetz, Winter, 2009
talks of Bongrand, Link & Kim
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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
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
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
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
NSI IN SNOVAE
Interplay between SN physics & neutrino properties
NU-NSI versus collective effectsRaffelt'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
THE BIG QUESTIONS
Singlet or 3plet fermionType-I & III
Triplettype-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 SEESAWInverse 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
EXPLAINING NEUTRINO PROPERTIES
Many models
Altarelli, Feruglio, MerloBabu et al,Barr et alFrampton et al,Grimus, LavouraHirsch et al ..King et al, Ross et alMa, Mohapatra et al,Plentinger & Rodejohan, Tanimoto, Raby et al, Ross et al,Zhang, ...
TBM ansatz Harrison–Perkins–ScottKing
Babu et al PLB552 (2003) 207Hirsch et al PRD69 (2004) 093006
Antusch, Kersten, Lindner, Ratz, Schmidt, 2005
JV16
Seesaw scale may be low
even within unification
JV17
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) 151802PRD79:016001,2009.
PRD72, 091301 (2005)
JV18
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
MERCI
next slides are backup
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DBD & FLAVOR
A4
PRD78:093007 (2008)
PRL 99 (2007) 151802
PRD72, 091301 (2005)
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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
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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)
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Hirsch et al PRD 78 (2008) 013006, Esteves et al JHEP05 (2009) 3
HIGH-SCALE SEESAWSUSY LFV DECAYS@LHC
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