Neutrino physics. Evgeny Akhmedov. Max-Planck-Institut für Kernphysik, Heidelberg & Kurchatov Institute, Moscow

Size: px

Start display at page:

Download "Neutrino physics. Evgeny Akhmedov. Max-Planck-Institut für Kernphysik, Heidelberg & Kurchatov Institute, Moscow"

Shanon Martin
5 years ago
Views:

1 Neutrino physics Experimental results and future Evgeny Akhmedov Max-Planck-Institut für Kernphysik, Heidelberg & Kurchatov Institute, Moscow Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 1/72

2 Atmospheric neutrinos Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 2/72

3 II. Neutrino experiments 17 Atmospheric neutrinos Atmospheric neutrinos are produced by the interaction of cosmic rays (p, He,... ) with the Earth s atmosphere: 1 A cr + A air π ±,K ±,K 0,... 2 π ± µ ± + ν µ, 3 µ ± e ± + ν e + ν µ ; at the detector, some ν interacts and produces a charged lepton, which is observed. _ π + ν µ π ( ) ν µ -+ ν ( ) ( ) e N π + _ µ +_ p, He e +_ Nν+ µ R µ/e = N + ν e N ν νµ N ν e ~ 2 M. Maltoni <maltoni@insti.physics.sunysb.edu> XXXIII ITEP WINTER SCHOOL, 28/02/2005 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 3/72

4 Super-Kamiokande detector Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 4/72

5 II. Neutrino experiments 18 Classification of atmospheric neutrino events Neutrino events are classified according to whether the track of the charged lepton begins and ends inside or outside the detector: end inside end outside begin inside fully contained partially contained begin outside stopping µ thru-going µ contained events are further divided into sub-gev and multi-gev data, depending on the reconstructed lepton energy E ν ν e,µ CONTAINED e,µ Fully Contained µ ν µ Partially Contained UPGOING MUONS µ µ νµ ν µ Stopping Thru-going Muon Muon few GeV few GeV few 10 GeV few 100 GeV dn/dlne, (Kt.yr) sub GeV multi GeV stopping muons through-going muons E ν, GeV (m.yr.ster) 2-1 M. Maltoni <maltoni@insti.physics.sunysb.edu> XXXIII ITEP WINTER SCHOOL, 28/02/2005 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 5/72

6 P<400MeV/c P>400MeV/c µ Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 6/72 11

7 Atmospheric neutrinos: Consistent with ν µ ν τ oscillations Oscillations of ν e may also be present at some level Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 7/72

8 Accelerator confirmations of ν atm oscillations Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 8/72

9 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 9/72

10 No-oscillation hypothesis excluded at 99.99% C.L. Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 10/72

The MINOS Experiment Main Injector Neutrino Oscillation Search

experiment at the atmospheric m2 One ν µ beam: NuMI 120 GeV

Detector: measure beam composition and spectrum Far Detector:

11 The MINOS Experiment Main Injector Neutrino Oscillation Search Accelerator-based long-baseline neutrino experiment Precision experiment at the atmospheric m2 One ν µ beam: NuMI 120 GeV protons from Fermilab Main Injector Two detectors Near Detector: measure beam composition and spectrum Far Detector: search for evidence of oscillations 735 km Far Detector Near Detector E. Falk Harris, U. Sussex SNOW 2006 Stockholm Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 11/72

12 ν µ ν µ ν µ ( ) = 2 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 12/72

13 ν µ σ ν µ σ ν µ σ Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 13/72

14 χ θ = + = = Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 14/72

15 Solar neutrinos Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 15/72

16 Fusion reactions: pp-cycle Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 16/72

17 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 17/72

18 II. Neutrino experiments 12 Homestake (South Dakota, USA): (44.35 N, 615 tons, 1970) SAGE (Baksan, Russia): (43.3 N, tons, 1990) Solar neutrino experiments GALLEX/GNO (LNGS, Italy): (42.5 N, 30 tons, 1991) Radiochemical SSM: 7 Be =13%, 8 B =78%; Reaction: ν e + 37 Cl 37 Ar+ e ; Threshold: MeV; Rate:2.56 ±0.16 ±0.16SNU. SSM: pp =54%, 7 Be =26%, 8 B =11%; Reaction: ν e + 71 Ga 71 Ge+e ; Threshold: MeV; Rate: SNU =10 36 captures/atom/sec SNU. SSM: pp =54%, 7 Be =26%, 8 B =11%; Reaction: ν e + 71 Ga 71 Ge+e ; Threshold: MeV; Rate: SNU. Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 18/72

19 II. Neutrino experiments 13 Kamiokande (Japan): (36.5 N, 1000 tons, ) Super Kamiokande (Japan): (36.5 N, tons, 1996) SNO (Sudbury, Canada): (46.5 N, 1000 tons, 1999) Solar neutrino experiments Water Cerenkov { Threshold: 7.5 MeV; { Flux: (2.80 ±0.19 ±0.33) 10 6 cm 2 s 1. Threshold:6.5MeV 5.0MeV; Flux: (2.32 ±0.03 ±0.08) 10 6 cm 2 s 1. Reaction: CC: ν e + d p+ p+e, NC: ν x + d n+ p+ν x, ES: ν x + e ν x + e ; Threshold:6.75MeV 5.0MeV; Flux: CC: ( ) 106 cm 2 s 1, NC: ( ) 106 cm 2 s 1, ES: ( ) 106 cm 2 s 1. Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 19/72

20 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 20/72

21 m 2 in ev Cl Ga SNO SuperK m 2 in ev KamLAND Cl 95% exclusion by rate Ga SNO KamLAND 95% allowed by rate+shape SuperK tan 2 (Θ) tan 2 (Θ) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 21/72

22 Super-Kamiokande Kamiokande-I I solar neutrino data May 31, 1996 July 13, 2001 (1496 days ) + e- + e- 8B flux : [x 106 /cm2/sec] Data = SSM(BP2004) solar events (14.5 events/day) ( Data/SSM(BP2000) = / ) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 22/72

23 Seeing the Sun underground The Sun still shines! Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 23/72

24 Energy spectrum of SK-I (tan2, m2) Best fit solar+kamland (as of before 2004) Energy correlated systematic error Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 24/72

25 SK-I day/night difference A DN = (Day-Night) (Day+Night)/2 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 25/72

26 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 26/72

27 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 27/72

28 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 28/72

29 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 29/72

30 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 30/72

Borexino is located under the Gran Sasso mountain which provides a shield against cosmic rays (4000 m water equivalent); Core of the detector: 278 tons of liquid scintillator contained in a nylon

31 Borexino is located under the Gran Sasso mountain which provides a shield against cosmic rays (4000 m water equivalent); Core of the detector: 278 tons of liquid scintillator contained in a nylon vessel of 4.25 m radius (PC+PPO); 1 st shield: 890 tons of ultra-pure buffer liquid (PC+quencher) contained in a stainless steel sphere of 6.75 m radius; External nylon vessel; it is a barrier against Rn emitted by PMT and s.steel 2214 photomultipliers pointing towards the center to view the light emitted by the scintillator (1843 with opt. concentr.) 2 nd shield: 2100 tons of ultra-pure water contained in a cylindrical dome; 200 PMTs mounted on the SSS pointing outwards to detect light emitted in the water by muons crossing the detector; Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 31/72

32 ν δ θ Predicted (SSM, no oscillations): 75 ± 4 counts/(day 100 ton) Observed: 47 ± 7 ± 12 counts/(day 100 ton) LMA MSW oscillations prediction: 49 ± 4 counts/(day 100 ton) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 32/72

33 Reactor ν e oscillations Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 33/72

34 CHOOZ and θ 13 δm 2 (ev 2 ) 1 Analysis A ν e ν x 90% CL Kamiokande (multi-gev) 90% CL Kamiokande (sub+multi-gev) % CL Search of reactor ν e disappearnce at L 1 km. No disappearance observed % CL sin 2 (2θ) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 34/72

35 . The general picture 44 Bound on θ 13 recent KamLAND and SNO-salt data help improving the sensitivity to θ 13 of solar data; however, present bound is still dominated by Chooz, together with atmospheric data; 3σ range:sin 2 θ KamLAND 2002 KamLAND 2004 Total m 2 31 [10 3 ev 2 ] % CL 3σ χ σ 90% CL Atm + K2K + Chooz Solar + KamLAND sin 2 θ 13 sin 2 θ 13 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 35/72

36 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 36/72

37 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 37/72

38 Expected: 1549 Background: 63 Observed: days, E th = 2.6 MeV R = N obs N bgr N expected = ± 0.020(stat) ± 0.026(syst) Stat. significance of reactor ν e disappearance: 8.5σ Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 38/72

39 Events / MeV Energy Spectrum above 0.9 MeV exposure : 2881 ton-year ( ton-year for KamLAND 2004 ) geo neutrinos previous result (above 2.6 MeV) preliminary KamLAND data no oscillation best-fit oscillation accidental C(,n) O Expected Geo e best-fit osci. + BG + Expected Geo e best-fit Geo + Reactor combined analysis No osci. expected Background (w/o geo neutrino) Observed events free parameter : geo neutrinos (U, Th) = (39.3, 29.4) events E prompt (MeV) goodness of fit using equal probability bins best-fit 2 / ndf = 21.0 / 16 (18.0% C.L.) no osci. 2 / ndf = 63.9 / 17 Scaled no oscillation spectrum is excluded at (Ichimura and Minekawa et al.) (tan 2, m 2 ) = (0.56, ev 2 ) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 39/72

40 Oscillation Parameters 2 ) 2 (ev 2 m small matter effect SNO KamLAND KamLAND 95% C.L. 99% C.L % C.L. best fit SNO 95% C.L. 99% C.L % C.L. best fit preliminary > 6 > tan KamLAND only tan 2 = 0.56 m 2 = ev 2 LMA II LMA (marginalized error) ) 2 ev -5 (10 2 m neutrino effect 3 neutino 2 neutino preliminary sin 12 same result for m 2 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 40/72

41 Precise measurement of m 2 ) 2 (ev KamLAND tan 2 = KamLAND + Solar 95% C.L. 99% C.L % C.L. global best fit m 2 = ev 2 This result KamLAND + SNO tan 2 = m 2 = ev 2 m 2 : systematic uncertainty 2.0% dominated by linear energy scale uncertainty 2 m tan 2 ev 2 ) -5 (10 m preliminary KamLAND + SNO 95% C.L. 99% C.L % C.L. best fit tan 2 m 2 is measured at 2.8% precision by KamLAND Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 41/72

42 Evidence for the MSW effect V (x) a MSW V (x); a MSW = 1 strongly favoured Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 42/72

43 The solar neutrino problem solved in reactor neutrino experiment! KamLAND: Identified the LMA MSW solution of the SNP Greatly reduced the uncertainty in m 2 Ruled out alternative solutions (neutrino magnetic moment,...) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 43/72

44 Oscillatory nature of ν µ disappearance in SK (atm) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 44/72

45 SK-I+II m 2 (ev 2 ) χ χ χ = ( χ χ ( 2 θ ν µ ν τ χ σ Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 45/72 13

46 Oscillatory nature of ν e disappearance at KamLAND Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 46/72

47 KamLAND 2004 (515 days) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 47/72

48 Neutrino Oscillation previous result (above 2.6 MeV) short baseline experiment Ratio 1.4 KamLAND data CHOOZ data best-fit osci. best-fit osci. + Expected Geo e st 2nd 3rd preliminary L 0 /E e (km/mev) KamLAND covers the 2nd and 3rd maximum characteristic of neutrino oscillation hypothetical single reactor at 180 km Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 48/72

49 Alternate Hypothesis previous result (above 2.6 MeV) V. D. Barger et al., Phys. Rev. Lett. 82, 2640 (1999) E. Lisi et al, Phys. Rev. Lett. 85, 1166 (2000) 1.4 KamLAND data CHOOZ data best-fit osci. best-fit osci. + Expected Geo e st 2nd 3rd Ratio preliminary oscillation decoherence 2 = 45.0 decay 2 = L 0 /E e (km/mev) best model is neutrino oscillation Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 49/72

I. Neutrino oscillations 39 The LSND experiment The only short distance signal for oscillation: L =30 m with E ν 30 MeV; Used the proton beam of Los Alamos.

50 I. Neutrino oscillations 39 The LSND experiment The only short distance signal for oscillation: L =30 m with E ν 30 MeV; Used the proton beam of Los Alamos. Same production chain as in ATM: 1 p+target π + + X, 2 π + µ + + ν µ, 3 µ + e + + ν e + ν µ ; observed ν µ ν e with probability P eµ = (0.26± 0.07 ±0.05)% Karmen which searched for the same signal and did not observe oscillations. MiniBOONE in Fermilab is running to solve this. Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 50/72

51 With 3 different m 2 4 light neutrinos needed! 4th ν: cannot be active must be sterile. Mixing matrix: 6 θ ij, 3 Dirac-type CP phases. But: simplifications occur only two possible type of schemes: 2+2 and 3+1 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 51/72

52 MiniBooNE was Prompted by the Positive LSND Result 3 LSND observed a (~3.8σ) excess of ν e events in a pure ν µ beam: 87.9 ± 22.4 ± 6.0 events Oscillation Probability: ( ν ν ) = (0.264 ± ± 0.045)% P µ e The Karmen Exp. did not confirm the LSND oscillations but had a smaller distance LSND in conjunction with the atmospheric and solar oscillation results needed more than 3 ν s Models developed with 2 sterile ν s or Other new physics models 3+2 models m 5 (Sorel, Conrad, and Shaevitz, PRD 70(2004) (hep-ph/ ) Karagiorgi et al., PRD75(2007) (hep-ph/ ) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 52/72

53 Summary 35 MiniBooNE rules out (to 98%CL) the LSND result interpreted as ν µ ν oscillations described with standard L/E dependence (Phys. Rev. Lett. 98, (2007), arxiv: v2 [hep-ex]) This eliminates the following interpretations of LSND: ν µ ν oscillations with (w/ standard assumptions of CP, E-dependence) ν µ ν via a single sterile neutrino ( ) The as-yet-unexplained deviation of MiniBooNE data from prediction at low-energy could be a background... Currently working on this with high priority... Or perhaps, new physics Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 53/72

54 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 54/72

55 Future neutrino experiments Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 55/72

56 What would we like to learn from future ν experiments? Explore the quantities that are not yet known (U e3, δ CP, sign of m 2 31) Improve the accuracy of already known parameters ( m 2 21, θ 21, m 2 31, θ 23 ) Study matter effects Study (discover or put limits on) non-standard neutrino interactions/mass varying neutrinos, etc. Dirac vs Majorana nature of ν 2β0ν decay experiments (GERDA, Majorana, Cuore,...) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 56/72

57 Absolute neutrino mass scale (direct ν mass measurements KATRIN ; cosmology) Precision measurement of leptonic parameters is in the agenda! Ultimate goal Unravel physics underlying neutrino mass generation Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 57/72

58 Why study U_e3 (A hymn to U e3 ) The least known of leptonic mixing parameters Discriminates between various neutrino mass models (Barr & Dorsner, 2000; Tanimoto, 2001,...) Unexplained smallness (rel. to m 2 / m 2 atm?) The (likely) bottleneck for studying fundamental CP and T effects and matter-induced T in neutrino oscillations Important for measuring the sign of m 2 31 in future LBL experiments normal vs inverted ν mass hierarchy Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 58/72

59 A hymn to U_e3 contd. Governs subdominant oscillations of atmospheric neutrinos in multi-gev region and interf. term in sub-gev region Governs the Earth matter effects on supernova neutrino oscillations The only opportunity to see the canonical MSW effect (strong matter enhancement of small mixing)? Drives the parametric enhancement of oscillations of core-crossing neutrinos inside the Earth Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 59/72

60 Future low-e ν experiments KamLAND-S, LENA, LENS, MOON, CLEAN, XMASS, Heron, Hallaz... Goals: Solar neutrino spectroscopy (currently < 0.01% of ν detected). Improving our knowledge of the solar energy production Studying matter dominated vacuum dominated transition in the dynamics of solar neutrino oscillations Improving considerably the accuracy of θ 12 Studying possible subdominant transition effects (RSFP, NSI, MaVaN) Improving the limits on U e3 (different correlation with θ 12 ) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 60/72

61 Future accelerator experiments Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 61/72

62 Conventional beams and super-beams p + A π ± (K ± ) + X π ± µ ± (e ± ) + ν µ (ν e ) Mainly ν µ ( ν µ ) with small admixture of ν e ( ν e ). Oscillations: ν µ ν e ν µ ν e Also ν µ disappearance (mainly ν µ ν τ ). possible but difficult. ν τ appearance Off-axis experiments (T2K, NOνA): reduce contamination by electron neutrinos and energy band at the expense of flux reduction. Sensitivity to CP, matter effects (sign of m 2 31) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 62/72

63 Neutrino factories Muon storage rings where muons are stored and decay in long straight sections: µ ± e ± + ν µ (ν µ ) + ν e ( ν e ) Possibility of sign flipping. Oscillations ( golden channels ): ν e ν µ ν e ν µ Clean beams: Appearance of wrong-sign muons clear signature. No contamination precision measurements Also silver channels : ν e ( ν e ) (ν τ ) ν τ ν fact.: Sensitivity to CP, matter effects. (sign of m 2 31 ) Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 63/72

64 Beta beams Intense beams of ν e or ν e produced in decays of highly accelerated (up to γ 100) β - radioctive nuclei ( 6 He, 18 Ne,...) Clean beams no flavour contamination Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 64/72

65 Degeneracies and correlations Degeneracies: to leading order osc. probabilities are invariant w.r.t. paramater transformations (8-fold degeneracy) : m 2 31 m 2 31 θ 23 π 2 θ 23 (θ 13, δ CP ) ambiguity Correlations: osc. probabilities depend on certain combinations of parameters. Example: (θ 12, θ 13 ) dependence of solar data. To resolve correlations and degeneracies combinations of different experiments necessary. Leads to some synergies a subject of intense study. Example: SBL reactor experiments free of (δ CP s 13 ) ambiguity combine with LBL data. Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 65/72

66 Future reactor experiments Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 66/72

67 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 67/72

68 Double Chooz existing far detector hall + another existing big hall! M. Lindner SNOW Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 68/72

69 Chooz Double Chooz and Triple Chooz FD only of DC Double Chooz Triple Chooz sin 2 2θ 13 sensitivity Chooz limit < 0.20 Double Chooz < 0.02 Triple Chooz? < Huber, Kopp, ML, Rolinec, Winter M. Lindner SNOW Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 69/72

70 Future Long Baseline Experiments K2K MINOS OPERA, ICARUS T2K NOνA T2H β-beams neutrino factory...muon collider analysis running construction approved pre-approved R&D R&D R&D... establish atmospheric oscillations with beam expected precision: 8% for m 2 13, 25% for sin2 θ 23, θ 13? 4% for m 2 13, 15% for sin2 θ 23, θ 13 3% for m 2 13, 15% for sin2 θ 23 (combined with T2K), θ 13, δ?, sgn( m 2 13 ) precision neutrino physics every stage is a necessary prerequisite for the next continuous line of improvements for beams, detectors, physics Manfred Lindner Group Seminar T30d, November Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 70/72

71 Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 71/72

72 Neutrino revolution continues! Evgeny Akhmedov Mainz U. Graduate School Meeting Bullay, Oct. 1-3, 2007 p. 72/72

Neutrino Experiments: Lecture 2 M. Shaevitz Columbia University

Neutrino Experiments: Lecture 2 M. Shaevitz Columbia University 1 Outline 2 Lecture 1: Experimental Neutrino Physics Neutrino Physics and Interactions Neutrino Mass Experiments Neutrino Sources/Beams and