Neutrino Oscillations
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1 Neutrino Oscillations Supervisor: Kai Schweda 5/18/2009 Johannes Stiller 1
2 Outline The Standard (Solar) Model Detecting Neutrinos The Solar Neutrino Problem Neutrino Oscillations Neutrino Interactions Sudbury Neutrino Observatory Data Collection & Results Conclusions & Outlook 6/27/09 Johannes Stiller 2
3 The Neutrino Introduced 1931 by Pauli Left-handed Fermion Spin 1/2 Lepton Flavored: e (1956) µ (1962)! (2000) Weak Interaction Cross Section: ~10-45 m 2 6/27/09 Johannes Stiller 3
4 The Standard Solar Model Includes Standard Model I.e. Luminosity and Radius Age dependent Nuclear Fusion Particle Propagation in the Sun Predicts Neutrino Flux: 6/27/09 Johannes Stiller 4
5 Neutrino Production in the Sun 6/27/09 Johannes Stiller 5
6 Outline The Standard (Solar) Model Detecting Neutrinos The Solar Neutrino Problem Neutrino Oscillations Neutrino Interactions Sudbury Neutrino Observatory Data Collection & Results Conclusions & Outlook 6/27/09 Johannes Stiller 6
7 Today: The Homestake Experiment Detecting Neutrinos Raymond Davis (Part of Nobel Price 2002) Total Solar Neutrino Flux 1478 m below Surface 615 Tons C 2 Cl 4 (Percloroethylene) 814 kev Threshold Energy Most sensitive to pep Reaction Only 1/3 of the Prediction!!! 6/27/09 Johannes Stiller 7
8 History: Probing the SSM : SAGE 50 Tons of Gallium : GALLEX Now: GNO 101 Tons Galliumtrichlorid Today: Super Kamiokande Photomultipliers Tons Pure Water Today: Sudbury Neutrino Observatory Tons D 2 O 6/27/09 Johannes Stiller 8
9 Outline The Standard (Solar) Model Detecting Neutrinos The Solar Neutrino Problem Neutrino Oscillations Neutrino Interactions Sudbury Neutrino Observatory Data Collection & Results Conclusions & Outlook 6/27/09 Johannes Stiller 9
10 The Solar Neutrino Problem Up to 70% of the predicted " e s missing! Some Mechanism must have changed their Flavor! 6/27/09 Johannes Stiller 10
11 Outline The Standard (Solar) Model Detecting Neutrinos The Solar Neutrino Problem Neutrino Oscillations Neutrino Interactions Sudbury Neutrino Observatory Data Collection & Results Conclusions & Outlook 6/27/09 Johannes Stiller 11
12 Neutrino Oscillations Weak Eigenstates (n=3): (n=2): Three Two Neutrino Analysis Mass Eigenstates Transition Probability: 6/27/09 Johannes Stiller 12
13 Outline The Standard (Solar) Model Detecting Neutrinos The Solar Neutrino Problem Neutrino Oscillations Neutrino Interactions Sudbury Neutrino Observatory Data Collection & Results Conclusions & Outlook 6/27/09 Johannes Stiller 13
14 The Goal Comparison of the relative Seize and Rates of three exclusive Signals Charged Current Reaction Sensitive only to # e s Electron Scattering Sensitive to # e s and # µ! s Neutral Current Reaction Equally sensitive to all Neutrino Flavors Derive $(# e ) and $(# µ! ) from the total detected Flux 6/27/09 Johannes Stiller 14
15 Charged Current (CC) Reaction W boson exchanged e - ejected at speed of light Amount of light ~ energy SSM predicts 30 events per day 6/27/09 Johannes Stiller 15
16 Electron Scattering (ES) e - direction correlated to incident neutrino Dominated by e - neutrinos by factor of 6.5 SSM predicts 3 events per day - 6/27/09 Johannes Stiller 16
17 Neutral Current (NC) Reaction Releases single 6.35 MeV Photon As Charged Current: Unique to Heavy Water Equally sensitive to all Flavors Direct Measurement of Flux of all Neutrinos Cross Section only 0.5 mb 6/27/09 Johannes Stiller 17
18 The Solution 6/27/09 Johannes Stiller 18
19 Outline The Standard (Solar) Model Detecting Neutrinos The Solar Neutrino Problem Neutrino Oscillations Neutrino Interactions Sudbury Neutrino Observatory Data Collection & Results Conclusions & Outlook 6/27/09 Johannes Stiller 19
20 Sudbury Neutrino Observatory Located in Canada Near Sudbury, Ontario 1730 m below Sea Level Construction of SNO finished in 1999 About 3 cosmic µ s per Hour Identifies Neutrino Flux of all Flavors via Cherenkov Light 6/27/09 Johannes Stiller 20
21 Detector Layout Four Neck Photomultiplier Tubes Deployment System Acrylic Vessel 12 m Diameter 1000 Tons of D 2 0 Surrounded by 1700 Tons of light Water Support Sphere cm Photomultiplier Tubes 54% of 4! Surrounded by 5700 Tons of light Water 91 outward facing Photomultiplier Tubes 23 inward facing Photomultiplier Tubes 6/27/09 Johannes Stiller 21
22 Acrylic Vessel 12 m 18 m Support Sphere with Photomultiplier Tubes 6/27/09 Johannes Stiller 22
23 Photomultiplier Tubes Light Refractors 6/27/09 Johannes Stiller 23
24 Particle Identification # e Event Muon Event Compton Scattering Multiple Cones Diffuse Cherenkov Ring Sharp-edged Cherenkov Ring 6/27/09 Johannes Stiller 24
25 How does an event look like? # e Event Muon Event 6/27/09 Johannes Stiller 25
26 Outline The Standard (Solar) Model Detecting Neutrinos The Solar Neutrino Problem Neutrino Oscillations Neutrino Interactions Sudbury Neutrino Observatory Data Collection & Results Conclusions & Outlook 6/27/09 Johannes Stiller 26
27 Analysis Strategy Measure Sum of all Fluxes Maximum Likelihood Fit Single Fluxes as free Parameters Model must include: Neutrino Interactions Propagation of Particles and Optical Photons Behavior of the DAQ Detector Changes Acceptance Corrections, Capture Efficiency, 6/27/09 Johannes Stiller 27
28 Calibration Calibration at Different Positions Different Radioactive Sources, i.e. 16 N 6.13 MeV Photons Multi-Wavelength Laser PMT Timing Optical Parameters Laser Ball 6/27/09 Johannes Stiller 28
29 Cherenkov Light Characteristics % ij 0.75 rad < % ij < 1.45 rad 6/27/09 Johannes Stiller 29
30 Cherenkov Box Cuts Background Incorrect reconstructed Tracks 6/27/09 Johannes Stiller 30
31 Data Collection & Cuts N hit > 21 T eff > 5 MeV 6/27/09 Johannes Stiller 31
32 Extraction of the Signals Effective Kinetic Energy 8 Be Spectrum R AV Reconstructed CC: Radial Position ES: NC: CC: ES: NC: 6.25 MeV H 2 O D 2 O Reconstructed Direction of the Event CC: ES: NC: 6/27/09 Johannes Stiller 32
33 Results 6/27/09 Johannes Stiller 33
34 Mixing Parameters 6/27/09 Johannes Stiller 34
35 Outline The Standard (Solar) Model Detecting Neutrinos The Solar Neutrino Problem Neutrino Oscillations Neutrino Interactions Sudbury Neutrino Observatory Data Collection & Results Conclusions & Outlook 6/27/09 Johannes Stiller 35
36 Conclusions & Outlook Solar Neutrino Problem! Solved by SNO!!! Neutrino Interaction Understood (?)! Neutrino Oscillations! Day-Night-Asymmetry Neutrinos have Mass!!! Improved hep Neutrino Search New Fitting Algorithms and Techniques BOREXINO Detector for Low Energies Supernova Early Warning System 6/27/09 Johannes Stiller 36
37 Sources B.Aharmim et al. (SNO Collaboration), arxiv:nucl-ex/ v1 B. Aharmim et al. (SNO Collaboration), Phys. Rev. Lett. 101, (2008) B. Aharmim et al. (SNO Collaboration), arxiv:nucl-ex/ v1 M.C. Gonzalez-Garcia, arxiv:hep-ph/ v3 C. Howard (SNO Collaboration), arxiv: v /27/09 Johannes Stiller 37
38 Pictures hart.png 6/27/09 Johannes Stiller 38
39 BOREXINO 278 Tons of Liquid Scintillator Nylon Vessel (125 µm) cm Photomultipliers 13.7 m Diameter Support Sphere Running since May 2007 Measuring MeV 7 Be # s Found Transitions between High ( 8 B)-and See CERN Courier, Vol. 49, #5, p. 13 6/27/09 Johannes Stiller 39
40 Day-Night-Asymmetry Would be strong Evidence for Neutrino Oscillation Observable spectral Distortions Dependence on Solar Zenith Angle Interaction with Matter in the Earth Change of Oscillation Parameters: Path Length Electron Density 6/27/09 Johannes Stiller 40
41 Phases 1-3 Phase 1 Detector filled with D 2 O Nov May 2001 Phase 2: Salt-Water-Phase 2 Tons NaCl Jun Oct Phase 3: Neutral Current Detectors Nov Nov /27/09 Johannes Stiller 41
42 Phase I: Results CC: ES: NC: 6/27/09 Johannes Stiller 42
43 Phase 2: Adding NaCL June 2001 until October 2003 Adding ~2000 kg of NaCl Cross Section of 35 Cl is 44 b Total Energy Released 8.6 MeV Multiple Gamma Rays Enhances: Neutron Capture Efficiency threefold Peak shifts 1 MeV Upward Different Isotropy of PMTs Total Flux Measurement more precise 6/27/09 Johannes Stiller 43
44 Phase 3: Neutral Current Detection (NCD) Nov until Nov Again filled with D 2 O 36 Strings of 3 He Counters Ultra pure Nickel Four 4 He Strings Background Detection - Neutral Current Flux suppressed + Improved Mixing Angle Uncertainty + Event by Event Particle Identification 6/27/09 Johannes Stiller 44 26
45 Results Compared x10-5 ev 2 x10 6 cm -2 s -1 6/27/09 Johannes Stiller 45
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