Neutrino experiments and nonstandard interactions
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- Τρυφωσα Καραβίας
- 7 χρόνια πριν
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1 Neutrino experiments and nonstandard interactions p. 1 Neutrino experiments and nonstandard interactions Omar G. Miranda Romagnoli Cinvestav
2 Neutrino experiments and nonstandard interactions p. 2 Contents Neutrino flavors Neutrino oscillations Solar and atmospheric Neutrinos Beyond the Standard Model
3 Neutrino flavors Neutrino experiments and nonstandard interactions p. 3
4 Neutrino experiments and nonstandard interactions p. 4 Neutrino flavors For neutrinos coming from the decay: n p + e + ν we observe the reaction ν + p n + e + When neutrinos are coming from the decay: we observe the reaction π µ + ν ν + p n + µ +
5 Neutrino experiments and nonstandard interactions p. 5 Neutrino experiments without oscillations Muon neutrinos on nuclei CHARM, CDHS, NuTeV R ν = σ(ν µn ν µ X) σ(ν µ N µ X) Muon neutrinos on electrons CHARM II σ(ν µ e ν µ e )
6 Neutrino experiments and nonstandard interactions p. 6 Neutrino experiments without oscillations NuTeV PRL (22); NNPDF NPB (29); Bentz et al PLB (21) NuTeV [Bentz et al.] NuTeV [NNPDF Coll.] NuTeV SM [Global EW fit] sin 2 θ W [on-shell]
7 Neutrino experiments and nonstandard interactions p. 7 Neutrino experiments without oscillations Electron neutrinos on nuclei Bugey, Chooz... Electron neutrinos on electrons LAMPF, Irvine (Reines, Gurr, Sobel),..., MUNU, Texono σ(ν e e ν e e )
8 Neutrino experiments and nonstandard interactions p. 8 Neutrino experiments without oscillations Barranco, OGM, Rashba PLB (28): sin 2 θ W =.259 ±.25 TEXONO PRD (21): sin 2 θ W =.251 ±.39 χ global Irvine Krasnoyarsk Rovno LAMPF LSND MUNU 9 % C. L. 1 1 σ sin 2 θ W
9 Neutrino experiments and nonstandard interactions p. 9 Neutrino oscillations Pontecorvo (1957,1967), Maki, Nakagawa, Sakata (1962) Massive ν s : the massive states ν i (i=1,2,3) are not equal to the flavor states (weak interactions) ν a (e, µ, τ) ν a = i U ai ν i Time: t = ν a (x, t = ) = i U ai e ip ix ν i Time: t > ν a (x, t) = i U ai e ip ix ie i t ν i Ultrarrelativistic ν-s m i p i E i = m 2 i + p2 i p i + m2 i 2p i y x t ν a (x, t) = i U ai e i m 2 i 2p t i ν i
10 Neutrino experiments and nonstandard interactions p. 1 Two neutrinos conversion Probability ν e ν µ P νe ν µ (x) = sin 2 (2θ) sin 2 πx Losc oscillation lenght Losc 25 km ( ) ( ) E 1 5 ev 2 MeV m 2
11 Neutrino experiments and nonstandard interactions p. 11 Oscillations in matter Wolfenstein 1978, Mikheev & Smirnov 1985 Neutral currents (NC): exchange of Z Charge currents (CC): exchange of W ± V e = ( 2G F N e N ) n, V µ = V τ = ( 2G F N ) n 2 2 Evolution equation i d dt ν e ν µ = m2 4E cos 2θ + 2 G F N e m 2 4E sin 2θ m 2 4E sin2θ m 2 4E cos 2θ ν e ν µ..
12 Neutrino experiments and nonstandard interactions p. 12 Constant density case Conversion probabilitiy ν e ν µ : ( P(ν e ν µ ; L) = sin 2 2θ m sin 2 π L ) l m, Mixing angle in matter sin 2 2θ m = ( m 2 2E ) 2 sin 2 2θ ( m 2 2E cos 2θ 2G F N e )2 + ( m 2 2E ) 2 sin 2 2θ Resonance 2G F N e = m2 2E cos 2θ
13 Neutrino experiments and nonstandard interactions p. 13 Three families U = R 23 (θ 23 ; )R 13 (θ 13 ;δ)r 23 (θ 23 ; )P, R 13 (θ 13 ;δ) = cos θ 13 sinθ 13 e iδ 1. sin θ 13 e iδ cosθ 13 P = diag(e iα, e iβ, 1)
14 Neutrino experiments and nonstandard interactions p. 14 Three families c 12 c 13 s 12 c 13 s 13 e iδ (s 12 c 23 + c 12 s 23 s 13 e iδ ) (c 12 c 23 s 12 s 23 s 13 e iδ ) s 23 c 13 (s 12 s 23 c 12 c 23 s 13 e iδ ) (c 12 s 23 + s 12 c 23 s 13 e iδ ) c 23 c 13 P(ν α ν β ) = X δ αβ 4 X i>j R j + 2 X i>j I 2 Uαj U βj e i m 2 j L 2E = n o Uαi U αju βi Uβj sin 2 n o Uαi U αju βi Uβj sin m 2! ij 4E L! m2 ij 2E L (1)
15 The solar interior Neutrino experiments and nonstandard interactions p. 15
16 Neutrino experiments and nonstandard interactions p. 16 Nuclear reactions in the Sun p + p 2 H + e + + ν e p + e + p 2 H + ν e (pp) 99.6 % (pep).4 % 2 H + p 3 He + γ 85 % 3 He + 3 He 4 He + 2p 15 % 3 He + 4 He 7 Be + γ % 3 He + p 4 He + e + + ν e %.13 % 7 Be + e 7 Li + ν e 7 Be + p 8 B + γ ( 7 Be) ( 8 B) 7 Li + p 2 4 He 8 B 8 Be + e + + ν e 8 Be 2 4 He
17 Neutrino experiments and nonstandard interactions p. 17 solar neutrino spectrum Bahcall s home page
18 Neutrino experiments and nonstandard interactions p. 18 Homestake Experiment, R.Davis 68 ν e + 37 Cl e + 37 Ar Pontecorvo 46
19 Neutrino experiments and nonstandard interactions p. 19 Homestake Experiment, R. Davis 68 ν e + 37 Cl e + 37 Ar Pontecorvo 46
20 Neutrino experiments and nonstandard interactions p. 2 Super-Kamiokande ν e + e ν e + e and ν x + e ν x + e Event/day/bin 2 Super-Kamiokande θ Sun 5-2 MeV cos θ Sun
21 Neutrino experiments and nonstandard interactions p. 21 Super-Kamiokande Predicted 8 B neutrino flux: cm 2 s 1 Super-Kamiokande I PLB (22); PRD (26) φ = 2.35 ±.2 (stat ±.8 (syst) 1 6 cm 2 s 1 Super-Kamiokande II PRD (28) φ = 2.38 ±.5 (stat ±.16 (syst) 1 6 cm 2 s 1 Super-Kamiokande III PRD (211) φ = 2.32 ±.4 (stat ±.5 (syst) 1 6 cm 2 s 1
22 Neutrino experiments and nonstandard interactions p. 22 SNO 2 PRL ν e + d p+ p + e (CC), ν x + d p + n + ν x (NC), ν x + e ν x + e (ES). φ e = (stat.)+.9.9 (syst.) φ µτ = (stat.) (syst.) φ SNO NC = (stat.) (syst.)
23 Neutrino experiments and nonstandard interactions p. 23 SNO 2 Outer H 2 O Inner H 2 O D 2 O Acrlyic Vessel PSUP
24 Neutrino experiments and nonstandard interactions p. 24 SNO 2 s -1 ) 6 cm -2 (1 φ µτ SNO φ ES SNO φ CC SNO φ NC φ SSM φ e 6 (1-2 cm -1 s )
25 Neutrino experiments and nonstandard interactions p. 25 theory vs. experiment [Bahcall s home page]
26 Neutrino experiments and nonstandard interactions p. 26 solar neutrino spectrum Bahcall s home page
27 Neutrino experiments and nonstandard interactions p. 27 Borexino experiment survival probability ν e P ee : Be - Borexino pp - all solar 8. B - all solar All solar without Borexino MSW Prediction [MeV] Borexino PRL (211) E ν
28 Neutrino experiments and nonstandard interactions p. 28 SNO experiment P νe ν e 1σ band SNO Borexino 7 Be pp - All solar ν experiments Pνe νe SNO E ν (MeV)
29 KamLAND 2 PRL reactor neutrinos geo neutrinos accidentals 1 Events/.425 MeV MeV analysis threshold KamLAND data no oscillation best-fit oscillation sin 2 2θ = 1. m 2 = 6.9 x 1-5 ev Prompt Energy (MeV) ( ) ν e + p n + e + : P νe ν µ (x) = sin 2 (2θ) sin 2 m 2 4E x Neutrino experiments and nonstandard interactions p
30 Neutrino experiments and nonstandard interactions p. 3 KamLAND 2 PRL ) 2 (ev m Rate excluded Rate+Shape allowed LMA Palo Verde excluded Chooz excluded sin 2θ
31 Neutrino experiments and nonstandard interactions p. 31 SNO 2 log( m /ev ) (a) SMA LMA -7 LOW % CL 95% CL 99% CL 99.73% CL VAC log(tan θ)
32 Other solutions Barranco et al PRD (22) Neutrino experiments and nonstandard interactions p. 32
33 6σ 5σ 4 σ 3 1 2σ σ σ Data fit KamLAND PRL (28) 2 χ σ 3σ 2σ 1σ ) 2 (ev -4 1 KamLAND 95% C.L. 99% C.L % C.L. best fit m 2 21 Solar 95% C.L. 99% C.L % C.L. best fit tan 2 θ 12 m 2 = ev 2, tan 2 θ = χ 2 Neutrino experiments and nonstandard interactions p. 33
34 Neutrino experiments and nonstandard interactions p. 34 m 2 21 and sin 2 θ m 2 21 [ 1-5 ev 2 ] sin 2 θ 12 sin 2 θ 12 = , m2 21 = ev 2 Schwetz, Tortola, Valle New J.Phys. 13 (211) 634
35 Atmospheric Neutrinos Neutrino experiments and nonstandard interactions p. 35
36 Neutrino experiments and nonstandard interactions p. 36 Atmospheric Neutrinos We will have the decays: and π + µ + + ν µ µ + e + + ν e + ν µ π µ + ν µ µ e + ν e + ν µ
37 Neutrino experiments and nonstandard interactions p. 37 Atmospheric Neutrinos 3 2 Sub-GeV e-like P < 4 MeV/c 3 2 Sub-GeV µ-like P < 4 MeV/c 6 4 multi-ring Sub-GeV µ-like Number of Events Sub-GeV e-like 4 Sub-GeV µ-like multi-ring P > 4 MeV/c P > 4 MeV/c Multi-GeV µ-like Multi-GeV e-like Multi-GeV µ-like PC cosθ cosθ cosθ
38 Neutrino experiments and nonstandard interactions p. 38 Atmospheric Neutrinos Super-Kamiokande PRD (26)
39 Neutrino experiments and nonstandard interactions p. 39 Atmospheric Neutrinos Data/Prediction (null osc.) L/E (km/gev) Super-Kamiokande PRL (24)
40 Accelerator Neutrinos Neutrino experiments and nonstandard interactions p. 4
41 Neutrino experiments and nonstandard interactions p. 41 neutrino oscillations Schwetz, Tortola, Valle New J. Phys (211) 4 m 2 31 [ 1-3 ev 2 ] 3 2 MINOS global atmospheric sin 2 θ 23
42 Neutrino experiments and nonstandard interactions p. 42 neutrino oscillations Schwetz, Tortola, Valle New J. Phys (211) m 2 31 [1-3 ev 2 ] GLOBAL SK+K2K+MINOS Sol + Reactors 9% CL (2 dof) Reactors sin 2 θ 13
43 Neutrino experiments and nonstandard interactions p. 43 neutrino oscillations T2K PRL (211) π π/2 2 Δm23 > δ CP -π/2 Best fit to T2K data 68% CL 9% CL -π
44 Neutrino experiments and nonstandard interactions p. 44 neutrino oscillations Schwetz, Tortola, Valle New J. Phys (211) parameter best fit ±1σ 2σ 3σ m 2 21 [1 5 ev 2 ] m 2 31 [1 3 ev 2 ] ( ) ( ) ( ) sin 2 θ sin 2 θ ± sin θ δ π π π 2π
45 Neutrino experiments and nonstandard interactions p. 45 Nonstandar interactions Beside the Standard Model Lagrangian: L eff = 2 2G F ([ ν β γ ρ Ll β ][ fγ ρ Lf ] + h.c.) m2 2 2G F P,f,β g f P [ ν βγ ρ Lν β ][ fγ ρ Pf] 4E cos 2θ + 2G F N e m 2 4E sin 2θ m 2 4E sin2θ m 2 4E cos 2θ
46 Neutrino experiments and nonstandard interactions p. 46 Non Standard Interactions (NSI) Most extensions of the SM predict neutral current non-standard interactions (NSI) of neutrinos which can be either flavor preserving (FD or NU) or flavor-changing (FC). NSI effective Lagragian: L NSI eff = αβfp ε fp αβ 2 2G F ( ν α γ ρ Lν β )( fγ ρ Pf) e, u, d e, u, d Here α, β = e, µ, τ; f = e, u, d; P = L, R; L = (1 γ 5 )/2; R = (1 + γ 5 )/2
47 Neutrino experiments and nonstandard interactions p. 47 R/ p parity violating SUSY An example of non-standard neutrino-electron and neutrino quark interactions: L = λ ijk ẽ k R ( ν i L) c e j L + λ ijk d j L d k Rν i L +... Barger, Giudice & Han 89 See e.g. Roulet 91, Amanik et al 5
48 Solar ν Oscillations and NSI with quarks Neutrino experiments and nonstandard interactions p. 48
49 Neutrino experiments and nonstandard interactions p. 49 Solar ν Oscillations and NSI with quarks H NSI = 2G F N f ( ε ε ε ). with ε = sin θ 23 ε fv eτ ε = sin 2 θ 23 ε fv ττ ε fv ee and ε fv ττ = ε fl ττ + ε fr ττ
50 Neutrino experiments and nonstandard interactions p. 5 Non Standard Interactions H NSI = 2G F N f ( ε ε ε ). Mixing angle in matter + NSI ( ) m 2 2E sin 2θ + 2 2G F εn d tan 2θ m = m 2 2E cos 2θ 2G F N e +. 2G F ε N d Resonance m2 2E cos 2θ 2G F N e + 2G F ε N d =. ε > N e N d
51 Neutrino experiments and nonstandard interactions p. 51 Data fit OGM, Tortola, Valle JHEP 61:8,26 m 2 SOL [ev2 ] sin 2 θ SOL sin 2 θ SOL
52 Neutrino experiments and nonstandard interactions p. 52 Data fit Tortola, OGM, Valle, JHEP 61:8, m 2 SOL [ev2 ] LMA-I LMA- LMA-D sin 2 θ SOL sin 2 θ SOL
53 Neutrino experiments and nonstandard interactions p. 53 Nonstandar interactions χ σ m 2 SOL [1-5 ev 2 ] % CL sin 2 θ SOL m 2 SOL [ ev2 ] % CL 3σ sin 2 θ SOL χ 2 Escrihuela, Miranda, Tortola, Valle, Phys.Rev.D8:159,29
54 Neutrino experiments and nonstandard interactions p. 54 Predictions for the probability.7.6 global best fit BF without NSI BF dark side < P ee >.5.4 pp (all) 7 Be (Borexino) 8 B (Borexino).3 8 B (SNO) E [MeV]
55 Neutrino experiments and nonstandard interactions p. 55 NSI-d constraints from Solar + Kamland 2 15 χ % C.L. 9% C.L ε ε
56 Neutrino experiments and nonstandard interactions p. 56 NSI-d constraints from Solar + Kamland Palazzo, Valle PRD (29)
57 Neutrino experiments and nonstandard interactions p. 57 NSI-d constraints for ν e and ν τ R e = σ(ν en νx) + σ( ν e N νx) σ(ν e N ex) + σ( ν e N ēx) = ( g Le) + ( g Re ) Constraints from CHARM II experiment ε L ee.3 < ε L ee <.3 ε R ee.6 < ε R ee <.5 ε L eµ ε L eµ <.5 ε R eµ ε R eµ <.5 ε L eτ ε L eτ <.5 ε R eτ ε R eτ <.5 CHARM II Collaboration, P. Vilain et. al. Phys. Lett. B (1994) Davidson, Peña-Garay,Rius,Santamaria JHEP 33:11 (23) hep-ph/3293
58 Neutrino experiments and nonstandard interactions p. 58 NSI-d constraints for ν e ν + d ν + p + n SNO NC is proportional to g 2 A ǫ A = α=e,µ,τ P eα NC ǫ da αα, da ε ττ CHARM (99%CL) solar + KamLAND (99%CL) da ε ee
59 Neutrino experiments and nonstandard interactions p. 59 NSI-d constraints for ν µ R µ = σ(ν µn νx) + σ( ν µ N νx) σ(ν µ N µx) + σ( ν µ N µx) = ( g Lµ) + ( g Rµ ) NuTeV [Bentz et al.] NuTeV [NNPDF Coll.] NuTeV SM [Global EW fit] sin 2 θ W [on-shell] Escrihuela, Miranda, Tortola, Valle, PRD (211)
60 Neutrino experiments and nonstandard interactions p. 6 NSI-d constraints for ν µ R µ = σ(ν µn νx) + σ( ν µ N νx) σ(ν µ N µx) + σ( ν µ N µx) = ( g Lµ) + ( g Rµ ) NNPDF da ε µµ.5 qa ε µτ Bentz et al. -.5 CHARM + CDHS.5 1 dv ε µµ qv ε µτ Escrihuela, Miranda, Tortola, Valle, PRD (211)
61 Neutrino experiments and nonstandard interactions p. 61 NSI-d constraints for ν µ.2.1 NNPDF.1.5 da ε µµ da ε µµ -.1 Bentz et al dv ε µµ dv ε µµ
62 Neutrino experiments and nonstandard interactions p. 62 NSI-d constraints for ν µ Global with NuTeV reanalysis NSI with down NSI with up NU NU NNPDF Bentz at al..42 < ǫ dv µµ < < ǫ uv µµ < < ǫ da µµ < < ǫ ua µµ < < ǫ dv µµ < < ǫ uv µµ < < ǫ da µµ < < ǫ ua µµ <.14 FC FC NNPDF/Bentz et al..7 < ǫ dv µτ <.7.7 < ǫ uv µτ <.7.39 < ǫ da µτ < < ǫ ua µτ <.39 Escrihuela, Miranda, Tortola, Valle, PRD (211)
63 Neutrino experiments and nonstandard interactions p. 63 NSI-e Laboratory constraints Laboratory experiments: 1. Reactor neutrinos 2. LEP data (e + e ν νγ) 3. CHARM
64 Neutrino experiments and nonstandard interactions p. 64 The ν e e interaction σ(ν e e νe) = 2G2 F m ee ν π 2 4(1 + gl e + εel ee ) 2 + X ε el αe (ge R + εer ee ) α e X ε er αe 2 α e 3 5 Davidson, Peña-Garay,Rius,Santamaria JHEP 33:11 (23) hep-ph/3293:.7 < ε el ee <.1 1. < ε er ee <.5 at 9 % C L Berezhiani, Raghavan, Rossi PLB (22) hep-ph/111138:.15 < ε el ee < < ε er ee <.5 at 99 % C L
65 Neutrino experiments and nonstandard interactions p. 65 The ν e e interaction Experiment Energy (MeV) events measurement LSND ν e e σ = [1.1 ± 1.5] E νe (MeV) 1 45 cm 2 Irvine ν e e σ = [.86 ±.25] σ V A Irvine ν e e σ = [1.7 ±.44] σ V A Rovno ν e e σ = (1.26 ±.62) 1 44 cm 2 /fission MUNU ν e e ±.34 events day Tritium Reactor LSND g L g R
66 Neutrino experiments and nonstandard interactions p. 66 The ν µ e ν µ e interaction dσ theo CHARM dy = 2G2 F m e π E ν + g L 2 + α µ g 2 R + α µ ε L αµ 2 ε R αµ 2 (1 y) 2
67 Neutrino experiments and nonstandard interactions p. 67 The e + e ν νγ interaction σ theo LEP (s) = dx dc γ H(x,s γ ;s) σ theo (ŝ), H(x,s γ ;s) = 2α πxs γ [ ( 1 x ) 2 x 2 c 2 γ ], σ SM (s) = N νg 2 F 6π M4 Z (g2 R + g2 L ) s ˆ(s M 2 Z ) 2 + (M Z Γ Z ) 2 (! s + 2M 2 W + G 2 F π M2 W M2 W s + M 2 W s 2s s g L MZ 2 (s M2 Z ) " (s + M 2 W ) 2 (s MZ 2 )2 + (M Z Γ Z ) 2 s 2 log log s + M 2 W M 2 W s + M 2 W M 2 W!! M2 W s 3 2 #),
68 Neutrino experiments and nonstandard interactions p. 68 The e + e ν νγ interaction σ NU (s) = X α=e,µ,τ G 2 F 6π s + G2 F π εl eem 2 W σ FC (s) = X α β=e,µ,τ " (ε L αα) 2 + (ε R αα) 2 2(g L ε L αα + g R ε R MZ 2 αα) (s M2 Z ) # (s MZ 2 )2 + (M Z Γ Z ) 2 "! # (s + M 2 W ) 2 s + MW 2 s 2 log M2 W 3, s 2 G 2 F 6π s h (ε L αβ )2 + (ε R αβ )2i. M 2 W
69 Neutrino experiments and nonstandard interactions p. 69 Laboratory constraints L ε ee R ε ee L ε µµ R ε µµ L ε ττ R ε ττ Barranco, Miranda, Moura, Valle PRD
70 Neutrino experiments and nonstandard interactions p. 7 Laboratory constraints.5 ε ll L L,R ε µµ L,R ε ee -.5 L,R ε ττ ε ll R
71 Neutrino experiments and nonstandard interactions p. 71 Laboratory constraints Region at 9% C. L. one parameter previous limits ε L ee.14 < ε L ee <.9.3 < ε L ee <.8.5 < ε L ee <.1 ε R ee.3 < ε R ee <.18.4 < ε R ee <.15.4 < ε R ee <.14 ε L µµ.33 < ε L µµ <.55 εl µµ <.3 εl µµ <.3 ε R µµ.4 < ε R µµ <.53 ε R µµ <.3 ε R µµ <.3 ε L ττ.6 < ε L ττ <.4.5 < ε L ττ <.2 ε L ττ <.5 ε R ττ.4 < ε R ττ <.6.3 < ε R ττ <.4 ε R ττ <.5 Barranco, Miranda, Moura, Valle PRD
72 Neutrino experiments and nonstandard interactions p. 72 Solar neutrinos solar neutrinos could be sensitive to the NSI with electrons Propagation could be affected Detection could also be affected! especially in SuperKamiokande
73 Neutrino experiments and nonstandard interactions p. 73 Solar neutrinos ε el ee ε el ee ε el ee ε er ee -1 1 ε er ee -1 1 ε er ee Bolaños, OGM, Palazzo, Tortola, Valle PRD79:11312,29
74 Neutrino experiments and nonstandard interactions p. 74 Solar neutrinos ε el ττ ε el ττ ε el ττ ε er ττ ε er ττ ε er ττ Bolaños, Miranda, Palazzo, Tortola, Valle Phys.Rev.D79:11312,29
75 Neutrino experiments and nonstandard interactions p. 75 Solar neutrinos Solar analysis Laboratory Previous limits ε L ee.36 < ε L ee < < ε L ee <.9.5 < ε L ee <.1 ε R ee.27 < ε R ee <.59.3 < ε R ee <.18.4 < ε R ee <.14 ε L µµ.33 < ε L µµ <.55 εl µµ <.3 ε R µµ.4 < ε R µµ <.53 ε R µµ <.3 ε L ττ.16 < ε L ττ <.11.6 < ε L ττ <.4 ε L ττ <.5 ε R ττ 1.5 < ε R ττ <.31.4 < ε R ττ <.6 ε R ττ <.5 Bolaños, OGM, Palazzo, Tortola, Valle PRD79:11312,29
76 Neutrino experiments and nonstandard interactions p. 76 Improving NSI constraints ΦeΜ Ε eμ Coloma, Donini, López-Pavón, Minakata
77 Neutrino experiments and nonstandard interactions p. 77 Confusion problem for θ 13 R eµ A s B s 13 ǫ P + C ǫ 2 P + D ǫ Pǫ S + E ǫ 2 S + F s 13ǫ S ǫ S ǫ S eτ, ǫ P ǫ P eτ. Huber, Schwetz, Valle, PRD
78 Neutrino experiments and nonstandard interactions p. 78 Confusion problem for θ 13 Neutrino factory + two different neutrino detectors sin 2 2θ 13 and δ marginalized Input: δ = π/4 sin 2 2θ 13 =.1 ε ee = ε eτ = ε ττ = ε eτ ε eτ ε ττ km ε eτ ε eτ ε ττ km ε eτ σ 2 σ 3 σ ε eτ ε ee ε ττ ε ττ ε ee Combined Ribeiro, Minakata, Nunokawa, S. Uchinami, R. Zukanovich-Funchal JHEP 712:2,27.
79 Neutrino experiments and nonstandard interactions p. 79 Confusion problem for θ 13 Neutrino factory + two different neutrino detectors ε ee and ε eτ marginalized ε ττ and ε eτ marginalized ε ee and ε ττ marginalized 6 δ 4 2 Input: δ = 3π/2 sin 2 2θ 13 =.1 ε ee = ε eτ = ε ττ = 3 km 6 δ km 6 δ σ 2 σ 3 σ Combined sin 2 2θ Ribeiro, Minakata, Nunokawa, S. Uchinami, R. Zukanovich-Funchal JHEP 712:2,27.
80 Confusion problem for θ 13 Neutrino factory + two different neutrino detectors Ε m eτ sensitivity 3Σ Ε m eτ sensitivity 3Σ 12 1 Optimum for standard performance indicators Symmetry axis 12 1 Symmetry axis L2 km Magic baseline Ε m ΑΒ Ε m ΑΒ L2 km Magic baseline 4 Ε m ΑΒ 1 2. Ε m ΑΒ Ε m ΑΒ EΜ 25 GeV GLoBES 28 Ε m ΑΒ Ε m ΑΒ EΜ 5 GeV GLoBES L1 km L1 km 12 1 Ε m ΜΤ sensitivity 3Σ Symmetry axis 12 1 Ε m ΜΤ sensitivity 3Σ Symmetry axis L2 km 8 6 Magic baseline L2 km 8 6 Magic baseline EΜ 25 GeV GLoBES 28 2 EΜ 5 GeV GLoBES L1 km L1 km 12 1 Ε m ΤΤ sensitivity 3Σ Symmetry axis Ε m ΤΤ sensitivity 3Σ Symmetry axis L2 km 8 6 Magic baseline L2 km 8 6 Magic baseline EΜ 25 GeV GLoBES 28 2 EΜ 5 GeV GLoBES L1 km L1 km Kopp, Ota, Winter, PRD Neutrino experiments and nonstandard interactions p. 8
81 Neutrino experiments and nonstandard interactions p. 81 Improving NSI constraints [J. Barranco, OGM, T.I. Rashba JHEP 512:21 5] Neutrino-nuclei coherent scattering (for qr << 1) dσ dt = G2 F M 2π ((G V + G A ) 2 + (G V G A ) 2 1 T «2 `G 2 V E MT G2 A ν Eν 2 ), M is the nucleus mass; T recoil nucleus energy (from to T max = 2E 2 ν/(m + 2E ν )); E ν neutrino energy.
82 Neutrino experiments and nonstandard interactions p. 82 Coherent scattering.6 T th = 4eV.6 T th = 1eV uv ε ee uv ε ee Ge [9% C.L.] Ge [9% C.L.] 76 Ge [99%] 76 Ge [99%] Ge+ Si [9%] Ge+ Si [99%] Ge+ Si [9%] Ge+ Si [99%] dv ε ee dv ε ee J. Barranco, OGM, T.I. Rashba JHEP 512:21 5
83 Neutrino experiments and nonstandard interactions p. 83 Coherent scattering.6 T th = 4eV.6 T th = 1eV uv ε τe uv ε τe Ge [9% C.L.] Ge [9% C.L.] 76 Ge [99%] 76 Ge [99%] Ge+ 28 Si [9%] Ge+ 28 Si [9%] 76 Ge+ 28 Si [99%] 76 Ge+ 28 Si [99%] dv ε τe dv ε τe J. Barranco, OGM, T.I. Rashba JHEP 512:21 5
84 Neutrino experiments and nonstandard interactions p. 84 Estimated bounds on NSI from TEXONO-like experiment (Ge+Si).6 T th = 4eV.6 T th = 4eV.4.4 uv ε ee Ge [9% C.L.] 76 Ge [99%] 76 Ge+ 28 Si [9%] 76 Ge+ 28 Si [99%] dv ε ee uv ε τe Ge [9% C.L.] 76 Ge [99%] Ge+ Si [9%] Ge+ Si [99%] dv ε τe 76 Ge+ 28 Si Tth =4eV ǫ dv ee <.36 ǫ uv ee <.38 ǫ dv τe <.48 ǫ uv τe <.5.6 T th = 1eV.6 T th = 1eV Ge+ 28 Si Tth =1eV uv ε ee Ge [9% C.L.] 76 Ge [99%] Ge+ Si [9%] Ge+ Si [99%] uv ε τe Ge [9% C.L.] 76 Ge [99%] Ge+ Si [9%] Ge+ Si [99%] ǫ dv ee <.18 ǫ uv ee <.19 ǫ dv τe <.34 ǫ uv τe < dv ε ee dv ε τe
85 Conclusions The solar neutrino problem remained unsolved for more than 3 years. It was the motivation, together with the atmospheric neutrino puzzle, for several experiments that have allowed to get a better knowledge of the Standard Model and of the neutrino properties. Neutrino physics counts now with several experiments that are improving the measurements of neutrino parameters and it is expected that new generation experiments could give a clue of the direction for physics beyond the Standard Model. Although we now better the neutrino masses diferences and mixings, there are many open question. Neutrino experiments and nonstandard interactions p. 85
86 Neutrino experiments and nonstandard interactions p. 86 R-parity breaking Susy λ ijk L i L Lj LĒk R λ ijk Li L Qj L D k R, (2) ν 2 ẽ Rk e 1 ν 2 λ 2j1 e 1 ẽ Lj e 1 λ 21k λ 21k ν 2 e 1 λ 2j1 ν 2 a) b) J. Barranco, OGM, T.I. Rashba PRD (27)
87 Neutrino experiments and nonstandard interactions p. 87 R-parity breaking Susy J. Barranco, OGM, T I Rashba hep-ph/72175 λ d L 1j1-2 λ d R 11k λ d 2 L current limit 1j1 TEXONO 1 ev beta beam TEXONO 4 ev SPS mass*time/(m year) J. Barranco, OGM, T.I. Rashba PRD (27)
Solar Neutrinos: Fluxes
Solar Neutrinos: Fluxes pp chain Sun shines by : 4 p 4 He + e + + ν e + γ Solar Standard Model Fluxes CNO cycle e + N 13 =0.707MeV He 4 C 1 C 13 p p p p N 15 N 14 He 4 O 15 O 16 e + =0.997MeV O17
LEPTONS. Mass m = ( ± ) 10 6 u Mass m = ± MeV me + m e
LEPTONS e J = 1 2 Mass m = (548.5799110 ± 0.0000012) 10 6 u Mass m = 0.510998902 ± 0.000000021 MeV me + m e /m < 8 10 9, CL = 90% qe + + q / e e < 4 10 8 Magnetic moment µ =1.001159652187 ± 0.000000000004
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