The elusive ν e. mass since Singapore Nov 27, 2008

Transcription

1 The elusive ν e mass since 1933 Singapore Nov 27, 2008

2 1 st Solvay Congress, Brussels Planck Solvay Lorentz Rutherford Onnes Einstein Nernst Curie Poincare Radiation & The Quanta, Autumn 1911

3 5 th Solvay Congress 1927 Compton De Broglie Born Ehrenfest Schrodinger Pauli Heisenberg Bohr Debye Dirac Planck Curie Lorentz Einstein Langevin Electrons & Photons

4 6 th Solvay Congress 1930 Stern Gerlach Brillouin Pauli Debye Fermi Heisenberg Dirac Zeeman Sommerfeld Einstein Bohr Curie Langevin Le Magnetisme

5 22 29 Octobre 1933 Heisenberg Fermi Dirac Debye Pauli Lawrence Schrodinger Bohr Curie Rutherford De Broglie Leitner 7th Solvay Congress, 1933 Structure et propriétés des noyaux atomiques

6 W. Pauli

7 Dear Radioactive Ladies and Gentlemen 4 Dec, 1930 there could exist in the nuclei electrically neutral particles, that I wish to call neutrons, which have spin and obey the exclusion principle

8 Dear Radioactive Ladies and Gentlemen, As the bearer of these lines, to whom I graciously ask you to listen, will explain to you in more detail, how because of the "wrong" statistics of the N and Li 6 nuclei and the continuous beta spectrum, I have hit upon a desperate remedy to save the "exchange theorem" of statistics and the law of conservation of energy. Namely, the possibility that there could exist in the nuclei electrically neutral particles, that I wish to call neutrons, which have spin 1/2 and obey the exclusion principle and which further differ from light quanta in that they do not travel with the velocity of light. The mass of the neutrons should be of the same order of magnitude as the electron mass and in any event not larger than 0.01 proton masses. The continuous beta spectrum would then become understandable by the assumption that in beta decay a neutron is emitted in addition to the electron such that the sum of the energies of the neutron and the electron is constant... I agree that my remedy could seem incredible because one should have seen those neutrons very earlier if they really exist. But only the one who dare can win and the difficult situation, due to the continuous structure of the beta spectrum, is lighted by a remark of my honoured predecessor, Mr Debye, who told me recently in Bruxelles: "Oh, It's well better not to think to this at all, like the new taxes". From now on, every solution to the issue must be discussed. Thus, dear radioactive people, look and judge. Unfortunately, I cannot appear in Tubingen personally since I am indispensable here in Zurich because of a ball on the night of 6/7 December. With my best regards to you, and also to Mr Back. Your humble servant. W. Pauli 3 Dec, 1930

9 22 29 Octobre 1933 Fermi Heisenberg Dirac Pauli Schrodinger Bohr

10 E. Fermi

11 E. Fermi s publications on the Weak Interaction E. Fermi, Tentative Theory of Beta Rays Letter Submitted to Nature (1933) 31 Dec, 1933 Published in Nuovo Cimento and Zeitschrift fur Physik Fm Stuart Freedman talk at Enrico Fermi Centennial Symposium 2001

12 Fermi s notes on QM Fermi s Golden Rule #2

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15 Fermi s Lectures on Nuclear Physics r(e) µ pe(e-e o ) 2 de

16 M. Koshiba Kamiokande neutrino detector

17 The Neutrinomass Experimental detection of neutrino oscillations Neutrinos have got mass How large is m(n e ), what is the mass hierarchy? 1. n-oscillations 7, ev 2 < Dm 122 < ev 2 solar 1, ev 2 < Dm 232 < ev 2 atm. There is a n with m ni 0,009eV and one with m nj 0,05eV 2. 0nbb-decay m(ne ) 0,4 ev to be confirmed 3. Tritium b-decay m(n e ) 2 = -0,6 2,2 2,1 ev 2 m(n e ) 2,3eV (95%) Mainz 4. Cosmology mni O(1eV) Talk by Beck at 2006 ICHEP

18 three roads to neutrino masses

19 The Neutrinomass Planned sensitivity of KATRIN: 0,2eV Detection limit 0,3eV (3s) / 0,35eV (5s)

20 Tritium β decay 3 H! 3 He + e + ¹º e

21 Tritium b-decay Tritium β Decay: 3 H 3 He + + e - + ν e Superallowed E 0 = 18.6 kev t 1/2 = 12.3 a dn/de = K F(E,Z) p E tot (E 0 -E e ) U ei 2 [ (E 0 -E e ) 2 m(ν i ) 2 ] 1/2

22 Kurie Plot vs Electron energy

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26 Overview of the KATRIN experiment Following slides taken from overview by G Drexlin at GERDA collaborators meeting, MPIK Heidelberg 2006

27 The KATRIN experiment KArlsruhe TRItium Neutrinoexperiment Being set-up at the Forschungszentrum Karlsruhe

28 G. Drexlin, FZ & University Karlsruhe Neutrino seminar / GERDA colla boration meeting, MPIK Heidelberg, February 21, 2006 The KATRIN experiment direct n-mass measurement with sub-ev sensitivity - astroparticle physics motivation - direct n-mass experiments - KATRIN components: source & spectrometers - sensitivity & outlook

29 history of tritium ß-decay results

30 simulated spectra at endpoint MC spectra for 1 full measuring year KATRIN scanning procedure: time per U 0

31 KATRIN time line 2001 first presentation, founding of KATRIN collaboration, LoI: hep-ex/ BMBF funding Astroteilchenphysik since 2002 background studies, R&D works, design optimisation 2003 pre-spectrometer manufacture, order for first large magnet group 2004 evaluation by HGF programme, Design Report 2004, orders for main spectrometer, WGTS & He-liquefier, 2005 vacuum tests pre-spectrometer 2006 electromagn. tests pre-spectrometer, main spectrometer on site 2007 source demonstrator, inner electrode mounting 2008 commissioning of WGTS, tritium loops, em. test of spectrometers 2009 system integration & first tritium runs regular data taking for 5-6 years (3fb years)

32 Summary measure absolute neutrino masses the growing excitement of neutrino physics KATRIN only model-independent approach with sub-ev sensitivity

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35 Main spectrometer aboard the vessel ANNEGRET at Constanta, Black Sea port On river barge Taifun passing Jochenstein lock on the Danube in Austria, with 7 cm. to spare!

36 Transport through village of Leopoldshafen Nov 24, 2006

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39 Chodos, Hauser, Kostelecky 1985

40 Phase Space Considerations

41 Kurie Plot vs Electron energy

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43 Chodos, Hauser, Kostelecky 1985

44 A Canonical Quantization N.P. Chang, Mod Phys Lett A 16, 2129 (2001)

45 Positive metric field Participates in Weak Interactions Negative metric field Sterile, only interact through Majorana mass mixing

46 Canonical Quantization

47 New Vacuum Structure With the properties

48 NJL structure of the vacua

49 < out jt(ã(x) Ã(y))j ¹ in >

50 Tritium Survival Amplitude

51 Cutkosky rule for normal mass

52 Cutkosky rule for tachyonic mass Transients with imaginary energy

53 Spacelike momenta Transients with Imaginary energy

54 Decay Spectrum (Tachyonic Neutrino) Transient Contribution

55 Electrons with x below the lower limit, - x res, would have energy E > E max

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60 Chodos, Hauser, Kostelecky 1985

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