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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. - PowerPoint PPT PresentationTRANSCRIPT
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http://ahep.uv.es
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OSCILLATION PARAMETERS CP VIOLATION & NSI
J W F ValleIFIC/CSIC – U Valencia
http://ahep.uv.es
JV1
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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
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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
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c.f. e.g. Fogli et al, 2008Lisi's talk
ZOOM Schwetz et al, NJP 10 (2008) 113
JV4
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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
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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
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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
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ROBUSTNESS wrt NU-NSI Escrihuela et al, arXiv:0907.2630 Miranda, et al JHEP 0610:008,2006.
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JV8
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Escrihuela et al, arXiv:0907.2630Miranda, et al JHEP 0610:008,2006.RESOLVING
Lowered threshold HE experimentsuseful SNO (LETA)SK-III Borexino
JV9
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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
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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
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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
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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
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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
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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
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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
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Seesaw scale may be low
even within unification
JV17
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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
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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
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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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