Solar Neutrinos & MSW Effect. Pouya Bakhti General Seminar Course Nov IPM
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1 Solar Neutrinos & MSW Effect Pouya Bakhti General Seminar Course Nov IPM
2 Outline Introduction Neutrino Oscillation Solar Neutrinos Solar Neutrino Experiments Conclusions Summary
3 Introduction
4 Introduction History Standard Model Neutrino Interactions Neutrino Sources
5 History 1914, Chadwick, β-spectrum continuous α- and γ-rays unique in energy
6 History N. Bohr: statistical energy conservation 1930, W. Pauli: neutron I have done something very bad today by proposing a particle that cannot be detected; it is something no theorist shouldever do. Wolfgang Pauli
7 History N. Bohr: statistical energy conservation 1930, W. Pauli: neutron 1933, E. Fermi: neutrino, massless 1942, Wang Ganchang: proposed detection 1956, Reines & Cowan: Detected
8 Standard Model wikipedia.org
9 Neutrino Interactions Charged Current Neutral Current Fundamentals of Neutrino Physics and Astrophysics, Carlo Giunti & Chung W. Kim.
10 Neutrino Interactions Electron + electron neutrino elastic scattering Fundamentals of Neutrino Physics and Astrophysics, Carlo Giunti & Chung W. Kim.
11 Neutrino Interactions Fundamentals of Neutrino Physics and Astrophysics, Carlo Giunti & Chung W. Kim.
12 Neutrino Sources Artificial Atmospheric Supernova Solar Big bang Geologic &...
13 Neutrino Oscillation
14 Neutrino Oscillation Mixing Neutrino Oscillations in vacuum Neutrino Oscillations in matter MSW effect
15 Mixing Flavour states & mass eigenstates PMNS mixing matrix Two neutrino mixing
16 Mixing Portrait of electron neutrino The MSW effect and Solar Neutrinos, A. Yu. Smirnov, arxiv:hep-ph/
17 Neutrino Oscillations in vacuum
18 Neutrino Oscillations in vacuum
19 Neutrino Oscillations in vacuum Two neutrinos
20 Neutrino Oscillations in vacuum Fundamentals of Neutrino Physics and Astrophysics, Carlo Giunti & Chung W. Kim.
21 Neutrino Oscillations in matter Coherent forward elastic scattering Fundamentals of Neutrino Physics and Astrophysics, Carlo Giunti & Chung W. Kim.
22 Neutrino Oscillations in matter
23 MSW effect
24 MSW effect The MSW effect and Solar Neutrinos, A. Yu. Smirnov, arxiv:hep-ph/
25 Solar Neutrinos
26 Solar Neutrinos Two type of thermonuclear reactions pp chain CNO cycle Standard Solar Model (SSM) Neutrinos
27 pp chain n pp n pep p + p 2 H + e + + n e 99,6% p + e - + p 2 H + n e 0,4% 2 H + p 3 He + g 85% 3 He + 3 He 4 He + 2p 15% He + p 4 He + e + + n e n hep 3 He + 4 He 7 Be + g 99,87% 0,13% 7 Be + e - 7 Li + n e n Be 7 Be + p 8 B + g 7 Li + p 4 He + 4 He 8 B 8 Be + e + + n e n B n B Solar neutrinos Recent results, Daniel Vignaud (APC Paris), 23 October Be 4 He + 4 He
28 CNO cycle Fundamentals of Neutrino Physics and Astrophysics, Carlo Giunti & Chung W. Kim.
29 SSM Neutrinos
30 SSM Neutrinos Solar Models: current epoch and time dependences, neutrinos, and helioseismological properties, John N. Bahcall, M. H. Pinsonneault, Sarbani Basu, arxiv:astro-ph/ v2
31 Solar Neutrino Experiments
32 Solar Neutrino Experiments Homestake experiment Gallium experiments KamiokaNDE Super-KamiokaNDE (SK) The Sudbury Neutrino Observatory (SNO)
33 Homestake experiment Proposed in 1964 Electron capture Auger electron wikipedia.org
34 Homestake experiment Located 1478 m below the surface volume of litters steel tank 6.1 m in diameter and 14.6 m long containing atoms of 37 Cl(133 ton) 615 ton of tetrachloroethylene C 2 Cl 4
35 Homestake experiment first data indicated in extraction from March 1970 to February 1994 Solar Neutrino Problem (SNP) Changes to the Solar Model
36 Gallium experiments GALLium EXperiment (GALLEX) Gallium Neutrino Observatory (GNO) The Soviet American Gallium Experiment (SAGE)
37 KamiokaNDE Kamioka Nucleon Decay Experiment Kamioka Neutrino Detection Experiment Water Cherenkov detector 1000 m underground Kamiokande-I, II, III E th = 9.0, 7.2, 6.7MeV
38 Kamiokande 3 kton water, 1000 PMTs Elastic scattering Sensitive to electron 8 B solar ν e s measured by Kamiokande is about half of the SSM flux
39 Super-Kamiokande 50 kton water PMTs
40 Solar Neutrino Experiments Fundamentals of Neutrino Physics and Astrophysics, Carlo Giunti & Chung W. Kim.
41 Super-Kamiokande Fundamentals of Neutrino Physics and Astrophysics, Carlo Giunti & Chung W. Kim.
42 SNO one kiloton of 99.92% isotopically pure D 2 O 9456 PMTs Fundamentals of Neutrino Physics and Astrophysics, Carlo Giunti & Chung W. Kim. Ryan Martin, Queen s University, Kingston, ON, Canada,8 th January EPFL
43 SNO detects through three reactions NC reaction on deuterium in important for checking the neutrino oscillation solution of the SNP
44 SNO D 2 O Phase NaCl Phase, 2 ton NaCl Third Phase hundred 3 He tubes σ( 35 Cl ) = 44 b σ( D ) = 0.5 mb George Ewan, for the SNO Collaboration Beyond the desert 2003
45 Salt phase SNO
46 Conclusions
47 Conclusions Vacuum oscillation disfavored no significant seasonal variation Resonance flavor transition Small Mixing Angle (SMA) Large Mixing Angle (LMA) Quasi-Vacuum Oscillation (QVO) LOW
48 Conclusions Allowed region in the tan2 ϑ-δm2 plane (LMA) obtained from a global analysis of solar neutrino data B. Aharmim et al., Phys. Rev., C72, , 2005, nucl-ex/ Fundamentals of Neutrino Physics and Astrophysics, Carlo Giunti & Chung W. Kim.
49 Conclusions Reactor experiment (KamLAND) + global solar neutrino data T. Araki et al., Phys. Rev. Lett., 94, , 2005, hepex/ Fundamentals of Neutrino Physics and Astrophysics, Carlo Giunti & Chung W. Kim.
50 Summary Neutrinos Neutrino oscillation Solar neutrinos Solar neutrino experiments & SNP Conclusions
51 Thanks for your attention
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