http://ahep.uv.es 1 oscillation parameters cp violation & nsi j w f valle ific/csic – u...

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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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