Neutrino Physics. Caren Hagner, Universität Hamburg

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1 Nutrino Physics Carn Hagnr, Univrsität Hamburg What ar nutrinos? Nutrino mass and mixing Nutrino oscillations Nutrino bams: OPERA Oscillation of acclrator nutrinos Solar Nutrinos: BOREXINO (KamLAND ractor nutrino xprimnt) Summary DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

2 Why ar w doing Nutrino Physics? Elmntary Particl Physics: - Mass? - Mattr antimattr symmtry - Physics byond th Standard Modl Cosmology: - arly univrs - structur formation - dark mattr Nutrino Physics Applications: - Monitoring of Nuclar Ractors - Go physics - Nw Tchnologis Astroparticl Physics: - Solar Nutrinos - Cosmic Radiation - Suprnova - Nutrino Tlscops

3 Fundamntal Particls Quarks: Lptons: u c t v v µ v τ d - s b µ - τ - Intractions by xchang of bosons: Graviton Photon Gluon W,Z DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

4 Wolfgang Pauli postulats th Nutrino (1930) Enrgy spctrum of lctrons from β-dcay n p E lctron Numbr of Elctrons = m c n On xpctd this Elctron nrgy But this was obsrvd! m p c E nutrino Solution: Th Nutrino DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

5 Wolfgang Pauli in Hamburg (1955) 195 Gnva 19 Assistant at Univrsität Hamburg 194 Habilitation in Hamburg (Discovry of th Exclusion Principl)

6 Dcay of th Nutron - Birth of a Nutrino Nutron Proton - Q Q=-1/3= /3 Q = -1/3 du v d n p u Q = /3 d u Transformation d-quark u-quark: Elctrowak Intraction! DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

7 Tritium β-dcay: Mainz/Troitsk 3 H 3 H - E 0 = 18.6 kv Mainz Data (1998,1999,001) m β = 1. ±. ±.1 V m < β.v ( 95%CL) DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

8 KATRIN: dlivry of vacuum vssl (008) m β Goal: < 0.0 V DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

9 Nutrino Proprtis Nutral Frmions with Spin ½ In th Standard Modl: masslss, stabl, always lft handd! BUT: Today w know that nutrinos hav mass 0.05 V < m v < V Standard Modl must b xtndd! Spin p v v L DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

10 Carn Hagnr, Univrsität Hamburg DESY Summr School 011 How Nutrinos intract Th wak intraction L L L b t s c d u L L L τ µ τ µ v W W v v µ W v µ µ W

11 Carn Hagnr, Univrsität Hamburg DESY Summr School 011 Chargd Currnt Exchang of a W Boson: v W d u W v µ µ v u u d d n p W µ v µ u d π

12 Nutral Currnt Exchang of a Z 0 Boson: v µ vµ v τ v τ n d u d Z 0 d u n Z 0 d DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

13 Carn Hagnr, Univrsität Hamburg DESY Summr School 011 Nutrino mass and mixing Nutrino mixing! Nutrino mixing! = τ τ τ µ µ µ τ µ U U U U U U U U U 3 massiv nutrinos: 1,, 3 with masss: m 1,m,m 3 Flavor-Eignstats v,v µ,v τ Mass-Eignstats Flavor-Eignstats v,v µ,v τ Mass-Eignstats v U v U v U v = Exampl:

14 Carn Hagnr, Univrsität Hamburg DESY Summr School 011 Paramtrisation of Nutrino Mixing Pontcorvo-Maki-Nakagawa-Sakata (PMNS) Matrix: 3 mixing angls: θ 1, θ 3, θ 13 1 Dirac-phas (CP violating): δ = δ δ τ µ c s s c c s s c c s s c i i θ sol θ 13, δ θ atm Θ 3 : 34 o - 58 o θ 13 <13 o, δ? θ 1 : 9 o - 39 o

15 Nutrino Mixing for Flavors µ = τ cosθ 3 sinθ 3 sinθ cosθ v θ µ = cos 3 v sin θ 3 v 3 Th probability that v µ has mass m is cos θ 3 mixing angl probability to hav a crtain mass Today w know that θ 3 45 o : v 1 v µ = ( v ) 3 v 1 v τ = ( v ).g. probability that v µ has mass m : 50% 3 DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

Nutrino Oscillations µ = cosθ 3 τ sinθ 3 sinθ cosθ 3 3 3 Flavor ignstats v µ, v τ Mass ignstats v,v 3 with m, m 3 sourc crats flavor-ignstats propagation dtrmind by

16 Nutrino Oscillations µ = cosθ 3 τ sinθ 3 sinθ cosθ Flavor ignstats v µ, v τ Mass ignstats v,v 3 with m, m 3 sourc crats flavor-ignstats propagation dtrmind by mass-ignstats v dtctor ss flavor-ignstats v µ v 3 v τ τ W W µ ω,3 = E,3 = p m,3 slightly diffrnt frquncis phas diffrnc changs p,n hadrons DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

17 Flavor Nutrino Oscillations Oscillation probability P( µ ) = sin τ (θ ) sin 3 π x L osz L osz.48 E (in GV) ( in km) = m (in V ) m = m m 3 Probability to find v τ L osz, m sin (θ) Distanc x in L osz DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

18 What do w know about nutrino masss? v v μ v τ m solar V, m atm 10-3 V V v 1 v v V v 3 Δm solar v v 1 Δm atm Δm atm Δm solar v v 1 v 3 normal hirarchy invrtd hirarchy quasi - dgnrat DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

Nutrino Important xprimntal Oscillations rsults wr in

V KK, MINOS, OPERA, TK atmosphric nutrinos acclrator

19 Nutrino Important xprimntal Oscillations rsults wr in rcnt obsrvd yars Nutrinos hav mass! JAPAN Supr-Kamiokand CANADA SNO JAPAN KamLAND v µ v τ,(s) Oscillation m 10-3 V v v µ,τ Oscillation m V KK, MINOS, OPERA, TK atmosphric nutrinos acclrator nutrinos Gallx/GNO, Sag, Supr-K, Homstak, BOREXINO solar nutrinos ractor nutrinos

20 Solar Nutrinos 4 p H MV 6.5E10 v /cm s Nutrino light from th Sun (Supr-Kamiokand)

21 Nutrino Production in th Sun: Th pp Cycl Carn Hagnr, Univrsität Hamburg Kolloquium Wupprtal,

22 Solar Nutrinos (E v MV) nrgy of th nutrinos in MV Th Sun in Nutrino Light (Supr-Kamiokand)

23 LNGS Masurmnt of Flux of 7 B Nutrinos (14m) t DESY Summr School m Carn Hagnr, Univrsität Hamburg

24 Dtction of solar nutrinos in BOREXINO: Elastic nutrino lctron scattring s v vx x (dominatd by v ) (Kinmatics lik Compton ffct),µ,τ,µ,τ t DESY Summr School 011 v can intract via CC NC v μ and v τ can only intract via NC! Carn Hagnr, Univrsität Hamburg

25 BOREXINO Expctd (lctron) nrgy distribution: 14 C (backgr.) 7 B CNO pp 8 B Edg at 665 kv DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

27 Photomultiplirs and light concntrators in Borxino

28 Borxino during filling (on top scintillator, lowr part watr)

29 Scintillator filling compltd May 15, 007

30 Borxino Rsult: Borxino Coll. prcision masurmnt of th 7B solar nutrino intraction rat in Borxino, arxiv: Carn Hagnr, Univrsität Hamburg Kolloquium Wupprtal,

31 What can w larn from this? 46 ± 1.5stat ± 1.6sys cpd/100 t Prdiction of standard solar modl: No oscillation 49 ± 3stat ± 4sys cpd/100 tons Oscillation (with θ 1 33 o ): high mtalicity Solar Modl low mtalicity Solar Modl 74 ± 5 cpd/100 t 47 ± 3 cpd/100t 44 ± 4 cpd/100 t No-Oscillation is xcludd from BOREXINO alon with mor than 4.9 sigma. φ( f ( B) B) f (pp) f 7 7 CNO = ( ) = φ( = ± 0.4 B) / φ SSM < 1.7%(95%CL) 10 9 cm s 1 = 0.97 ± 0.05(stat) ± 0.07(syst) Carn Hagnr, Univrsität Hamburg Kolloquium Wupprtal,

32 Summary of Nutrino Oscillations Nutrino Oscillations hav bn obsrvd with solar, atmosphric, ractor and acclrator nutrinos. Nutrinos hav mass! Th absolut nutrino mass has not yt bn masurd, allowd rang: 0.05 V < m v < V Nutrino mixing xists and is vry diffrnt from quark mixing. Why? Masurmnts of third mixing angl hav bn startd, hints that sin (θ 13 ) 0.0 (?). Is thr CP-violation for nutrinos? Is th nutrino a Majorana particl? Sarch for nutrinolss Doubl-Bta Dcay (Evidnc?) DESY Summr School 011 Carn Hagnr, Univrsität Hamburg

Antonio Pich. IFIC, CSIC Univ. Valencia.

Antonio Pich. IFIC, CSIC Univ. Valencia. Antonio Pich IFIC, CSIC Univ. Valncia Antonio.Pich@crn.ch Th Standard Modl A. Pich - CERN Summr Lcturs 2005 1. Constitunts & Intractions 2. Quarks 3. Gaug Invarianc 4. Quantum Chromodynamics 5. Elctrowak