Neutrino Physics II. Neutrino Phenomenology. Arcadi Santamaria. TAE 2014, Benasque, September 19, IFIC/Univ. València

Neutrino Physics II Neutrino Phenomenology Arcadi Santamaria IFIC/Univ. València TAE 2014, Benasque, September 19, 2014

Neutrino Physics II Outline 1 Neutrino oscillations phenomenology Solar neutrinos and KamLAND Atmospheric neutrinos and MINOS Results on θ 13 and global fits (Close) future: measurement of sign( m 2 31 ) and δ 2 Absolute Mass Scale Cosmological Bounds Beta and double beta decays 3 Other neutrino properties Limit on N ν Sterile ν s, NSI and magnetic moments Supernova neutrinos BAU from Leptogenesis

1 Neutrino oscillations phenomenology Solar neutrinos and KamLAND Atmospheric neutrinos and MINOS Results on θ 13 and global fits (Close) future: measurement of sign( m 2 31 ) and δ 2 Absolute Mass Scale 3 Other neutrino properties 4 Summary of neutrino properties 5 Conclusions

Solar neutrino experiments 6 Experiment Reaction Threshold Homestake ν e 37 Cl e 37 Ar E > 0.814 MeV SAGE, Gallex/GNO ν e 71 Ga e 71 Ge E > 0.233 MeV Super-Kamiokande ν e,x e ν e,x e E > 5.5 MeV SNO ES: ν e,x e ν e,x e CC: ν e D ppe NC: ν x D ν x pn E > 5.5 MeV s -1 cm -2 ) φ µτ ( 10 6 5 4 BS05 φssm 68% C.L. NC φµτ 68%, 95%, 99% C.L. 3 SNO φcc 68% C.L. 2 SNO φnc 68% C.L. SNO 1 φes 68% C.L. SK φes 68% C.L. 0 0 0.5 1 1.5 2 2.5 3 3.5 6 φ ( 10 cm -2 s -1 e ) Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 1/22

Tests with reactor neutrinos: KamLAND Terrestrial anti-neutrinos from nuclear reactors in Japan with E 1 MeV and average L 180Km ( m21 2 L/(4E) 1) ν e p e + n, E νe = E e + + m n m p Measurement of P( ν e ν e ) as a function of the energy! Survival Probability 1 0.8 0.6 0.4 Data - BG - Geo! e Expectation based on osci. parameters determined by KamLAND 0.2 0 20 30 40 50 60 70 80 90 100 L 0 /E!e (km/mev) Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 2/22

Global results 5 90% CL 0 15 solar m 2 21 [ 10-5 ev 2 ] 10 5 global KamLAND 0 0.2 0.4 0.6 0.8 sin 2 12 0 LMA MSW solution Oscillations ν e ν µ,τ Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 3/22

Atmospheric neutrino: SuperKamiokande π + µ + ν µ e + ν e ν µ ν µ. Same with π. If ν s are not distinguished from ν s: 2ν µ for each ν e Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 4/22

L 10 Km to 10 4 Km and E 0.1 GeV To 10 GeV. Ideal to have oscillations with m 2 10 3 ev 2. SuperKamiokande ν ei + N e i + N detects e i by Cherenkov: It does not see the charge It allows to obtain the direction of ν ei its energy and the flavour Results: ν e flux not changed and no dependence in L Oscillations ν µ ν x x τ (no much space for steriles or ν decays) Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 5/22

Test in accelerators SuperK results confirmed by neutrinos produced in accelerators: MINOS, K2K,Opera Opera: ν µ ν τ L = 732 Km E 17 GeV K2K: ν µ ν µ L = 250km E 1 GeV MINOS: ν µ ν µ L = 735km E 3 GeV Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 6/22

m 2 31 [ 10-3 ev 2 ] 3.5 3 2.5 2 90,99% CL MINOS T2K global Two solutions: m 2 31 > 0 Normal hierarchy (NH) m 2 31 < 0 Inverted hierarchy (IH) Octant ambiguity in θ 23 1.5 0.3 0.4 0.5 0.6 0.7 sin 2 θ 23 Oscillations ν µ ν τ Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 7/22

Results on θ 13 and δ θ 13 has been measured since 2012 to be different from zero by using reactor anti-neutrino disappearance (Daya Bay and RENO) as well as accelerator appearance and disappearance (MINOS and T2K) From Global fits some indirect information on δ Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 8/22

The two mass orderings Ν e Ν Μ Ν Τ Neutrino Mass Squared 2 m atm 2 m sol 3 sin 2 Θ13 2 1 sin 2 Θ12 sin 2 Θ23 NORMAL sinθ13 cos 1 1 1 1 1 1 sinθ13 2 m sol 2 m atm 2 1 3 sin 2 Θ13 sin 2 Θ12 sin 2 Θ23 sinθ13 INVERTED cos 1 1 1 1 sinθ13 1 1 Fractional Flavor Content varying cos m21 2 = 7.6 10 5 ev 2 (2.5% sin 2 θ 12 = 0.32 (4%) { m31 2 = 2.48 10 3 ev 2 sin 2 θ 23 = 0.57 (11%) 2.38 10 3 ev 2 (2.5%) sin 2 θ 13 = 0.021 (5%) Octant ambiguity in θ 23 δ still not well determinded from the fits but a hint for δ 3π/2 Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 9/22

(Close) future: measurement of sign( m 2 31 ) and δ Noνa (ν µ ν e And ν µ ν e ): sign( m 2 31 ) (Earth MSW effects) δ ( ν e vs ν e ) Strong dependece on θ 23 Also: ν-factories (NF), Super Beams (SB), Beta Beams (BB) Direct CP asymmetry A CP αβ (P(ν α ν β ) P( ν α ν β ))/(P(ν α ν β ) + P( ν α ν β )) difficult: depends on J = s 12 c 12 s 23 c 23 s 13 c13 2 sinδ and the two mass differences m21 2 and m2 31 Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 10/22

1 Neutrino oscillations phenomenology 2 Absolute Mass Scale Cosmological Bounds Beta and double beta decays 3 Other neutrino properties 4 Summary of neutrino properties 5 Conclusions

Cosmic Neutrino Background ν s decouple at T f 1MeV and present ν density is n ν = 3ζ (3)g ν 4π 2 T 3 ν 112cm 3, kt ν 10 4 ev if m ν 0, ν s contribute to the mass density of the universe Ω νi = n ν i m νi ρ c Ω ν h 2 = i m νi 94eV, h 0.7,Ω 0.3 m νi 14eV i Refined using CMB and LSS (depends on hypothesis) m νi < 0.2 2 ev i Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 11/22

Beta decay β decay of tritium: 3 H 3 He + e + ν e Very little available energy (order few kev) very sensitive to m ν dn de = U ei 2 Γ(m 2 ν i,e) = Γ(m 2 ν,e) Γ( m 2 ν,e) m 2 ν e m 2 ν = U ei 2 m 2 ν i = (M νm ν ) ee = c 2 13 (m2 1 c2 12 +m2 2 s2 12 )+m2 3 s2 13 3 Bound from MAINZ and TROITSK 1 in ev mνe 0.3 0.1 0.03 0.01 Sensitivity of KATRIN m 2 23 0 m 2 23 0 99 CL 1 dof 0.003 10 3 0.01 0.1 disfavoured by cosmology Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 12/22

Neutrinoless 2β decay 2νββ observed with T 2νββ 10 20 year 0νβ β requires Majorana ν masses (does not conserve LN) Suppressed by m ν but enhanced by phase space A 0νββ G 2 F m ββ q 2, q 100MeV m ββ = Vei 2 m i = ( ) VM diag V T = ( M ) ν = ee ee = c13 2 (m 1c12 2 + m 2s12 2 e2iα ) + m 3 s13 2 e2i(β δ) Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 13/22

Present limits (HM,IGEX) give m ββ 0.3 0.4eV. Improved recently by KamLAND-Zen (and EXO-200) m ββ 0.12 0.25eV Future (KamLAND2-Zen,nEXO,Majorana,GERDA2,CUORE,... ): m ββ 0.01eV Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 14/22

1 Neutrino oscillations phenomenology 2 Absolute Mass Scale 3 Other neutrino properties Limit on N ν Sterile ν s, NSI and magnetic moments Supernova neutrinos BAU from Leptogenesis 4 Summary of neutrino properties 5 Conclusions

Limit on N ν N ν = 2.982 ± 0.008 Light (m ν 45GeV) Active (full Z couplings) Any other light particle coupling to the Z will contribute A fourth generation with m ν4 < 45GeV: N ν = 1 (excluded) Triplet majorons (Y = 1): N ν = 2 (excluded) Doublet majorons, light sneutrinos: N ν = 1/2 (excluded) Light esterile (singlet) neutrinos are allowed Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 15/22

Sterile ν s, NSI and magnetic moments Sterile neutrinos LSND and MiniBoone see evidence of transitions ν µ ν e with mlsnd 2 > m2 ATM (Also hints from reactor, Gallium anomalies and from cosmology (N s = 1,2)) Experimental situation not completely clear Difficult to adjust everything Necessary, at least, a fourth neutrino (sterile given Γ Z ) Non-standar interactions (NSI) L NSI = ε fc αβ 2 2G F 2 ( ν α γ µ P L ν β )( f γ µ P L,R f ), affect ν cross sections and oscillations. Not very strong limits, typically ε αβ < 0.01 10 depending on the flavours. Neutrino magnetic moments Change νe νe cross section (µ ν 10 10 µ B ) and contribute to the energy loss of stars because plasmon decay γ P νν. From red giant stars µ ν < 3 10 12 µ B 2m ν < ω P 10KeV Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 16/22

Supernova neutrinos Energy released in a SN explosion 3 10 53 erg mainly neutrinos (99%) E ν few MeV. t 10s. The 3 types of neutrinos are emitted. SN1987A observed: 24 ν in a 13s interval. Limit on the masses: m ν < 16 ev Restrictions on the neutrino velocities Restrictions on non-standard cooling mechanisms Oscillation to steriles sin 2 2θ s 10 8 Magnetic moments of neutrinos Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 17/22

BAU from leptogenesis We exist!: η B (n baryons n antibaryons )/n γ 6 10 10. Sakharov: a) B 0, b) out of equilibrium c) C 0 & (CP) 0 Possible in the SM but not enough. In seesaw L B ε 1 = Γ(N 1 Φl) Γ(N 1 Φ l) Γ(N 1 Φl) + Γ(N 1 Φ l) N 1 Φ l ε 1 = 3 16π i + N 1 Φ l N Φ + l Im{( λ ν λ ν ) 2 i1 } M 1 ( λ λ) 11 M i 8 16π N 1 Φ l N M 1 v 2 m2 atm 1/2 Sphalerons conserve B L but violate B with L = B η B = 10 2 ε 1 κ M 1 10 9 GeV Φ l Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 18/22

1 Neutrino oscillations phenomenology 2 Absolute Mass Scale 3 Other neutrino properties 4 Summary of neutrino properties 5 Conclusions

Summary of parameters m 2 31 ±2.4 10 3 ev 2 θ 23 45 Atmos,K2K,MINOS m 2 21 7.6 10 5 ev 2 θ 12 35 Solar, KamLAND θ 13 9 T2K,MINOS,Double Chooz Daya Bay,RENO N ν (active and light) 3 LEP m ββ = i V 2 ei m ν i 0.2eV KamLAND-Zen,EXO,HM,IGEX,... m νe = i V ei 2 m 2 ν i < 2.2eV Mainz and Troitsk i m νi 1eV Cosmology sign( m 2 31 )? Noνa,NF,BB,SB,... CP, δ 3π/2? Noνa,NF,BB,SB,... Dirac or Majorana? (α,β)? HM?,0νβ β N s (light sterile) 1,2? LSND,MiniBooNE,Cosmology µ ν /µ B < 10 10,10 12 σ ν, red giants NSI ε 0.01 10 Sun,Atm,LSND,NF,... LFV (µ eγ, ) < 5.7 10 13 MEG,COMET/Mu2e,... Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 19/22

Unknowns m lightest not known (it could be zero) Mass ordering ( sign( m31 2 ) ) now known Is there CP violation (δ)? Is LN conserved in 2β decays? Is it due to Majorana ν masses? Is there LFV in the charged sector (µ eγ,τ µγ, µ-e conversion, ) Are there sterile ν s, NSI or magnetic moments? Why ν masses are so small? Why the structure of masses and mixings is so different from the quark sector? Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 20/22

1 Neutrino oscillations phenomenology 2 Absolute Mass Scale 3 Other neutrino properties 4 Summary of neutrino properties 5 Conclusions

Conclusions We have learned a lot on the neutrino properties in the last years but there is still a lot to be learned Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 21/22

Conclusions We have learned a lot on the neutrino properties in the last years but there is still a lot to be learned We do not have a Standard Model of neutrino masses but have many interesting ideas Fortunatelly, we have many proposed experiments which can refine our knowledge on the neutrino properties and guide us in our way to a Standard Model of Neutrino Masses Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 21/22

Thank you Thanks for your attention It has been a pleasure! Arcadi Santamaria Neutrino Physics II TAE 2014, Benasque, September 19, 2014 22/22