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Super-KamiokaNDE (Universe, Mankind and Neutrinos)

Super-KamiokaNDE (Universe, Mankind and Neutrinos). 2008-09-05 at Erice. Abstract :

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Super-KamiokaNDE (Universe, Mankind and Neutrinos)

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  1. Super-KamiokaNDE(Universe, Mankind and Neutrinos) 2008-09-05 at Erice Abstract: The recently known properties of the neutrinos will be summarized. Their relation to the Mankind as well as to the Universe will be discussed. Future possibilities with the neutrinos will alsobe discussed. M. Koshiba

  2. (1) We have 3 families of elementary particles each consisting of 16 members. See next slide. Each of these has its anti-particle, and this makes the total number of elementary particles equal to 96. Large number indeed. Most of them are electrically charged and only the neutrinos are neutral and this makes them extremely difficult to observe. They are very penetrating and makes it possible to observe the stellar interior; X-rays make the bones visible. (2) We have three topics in this lecture. Namely, the supernova neutrinos, the solar neutrinos and the neutrino oscillation. Before discussing these neutrino topics, we spend sometime explaining what we know about the neutrinos. The92 chemical elements to form our bodies: where and how were they created? Can we see the real beginning of Big-Bang?

  3. uL, uL, uL, dL, dL, dL, eL neL uR, uR, uR, dR, dR, dR, eR neR 1st Family or e-Family cL, cL, cL, sL, sL, sL, mL nmL cR, cR, cR, sR, sR, sR, mR nmR 2nd Family or m-Family tL, tL, tL, bL, bL, bL, tL ntL tR, tR, tR, bR, bR, bR, tR ntR 3rd Family or t-Family 4 Interactions and 4 mediating Bosons Strong Interaction on colored Quarks and Gluons, g. E-M interaction on charged particles and Photon, g. Weak Interaction and Z0,W+-. Gravitational Interaction on all and Gravitons.

  4. W.Pauli Introduction of neutrino W.Pauli; Letter to L.Meitner and her colleagues (letter open to the participants of the conference in Tubingen) (1930).

  5. Majorana neutrino Ettore Majorana Nuovo Cim. 14 (1937) 171-184. The possibility raised. neutrino=anti-neutrino Still unsetteled problem. Relevant experiment is bbdecay.

  6. F.Reines and C.Cowan

  7. Detectors by Reines and Cowan Observation of anti-ne from the nuclear reactor. F.Reines and C.L.Cowan, Phys. Rev. 92 (1953) 830. F.Reines and C.L.Cowan, Phys. Rev. 113 (1959) 273. 3 events observed

  8. B.Pontecorvo Neutrino oscillation hypothesis B.Pontecorvo, Zh. Eksp. Teor. Fiz. 53 (1967) 1717 [Sov. Phys. JETP 26 (1968) 984]. .

  9. Maki, Nakagawa, Sakata Possibility of neutrino oscillation pointed out. Z.Maki, M.Nakagawa, and S.Sakata, Prog. Theo. Phys. 28 (1962) 870. S.Sakata Z.Maki

  10. J.Steinberger, M.Schwartz and L.Lederman Discovery of nm different from ne

  11. Discovery of muon neutrinos, nm Neutrino detector G.Danby et al., Phys. Rev. Lett. 9 (1962) 36. muon ν Observed event

  12. Observation ofnt (DONUT collaboration)

  13. Observation ofnt K.Kodama et al., Phys. Lett. B 504 (2001) 218. 2 examples of nt candidates

  14. 3 kinds of neutrinos do exist. • Are there any more? The answer is NO from the shape of Z0 meson decay observed in LEP experiments. • What role do they play in the Universe? • What can they tell us about the Universe? • What physical properties do they have? • And so on.

  15. The sun is emitting ne. • In the inner part of the sun the nuclear fusion process, 4p to 4He, is going on. Namely 2 ne s per 1 4He are emitted; p changes to n + e-+ ne. The flux is reliably estimated from the observed solar energy flux. • The next slide shows the estimated solar neutrino energy spectrum together with the summary of the neutrino flux measurements.

  16. Summary of the Solar neutrino data Rate measurements @ Neutrino 2002 Target Data / SSM (BP2000.2) ・ Homestake 37Cl 0.34±0.03 ・ SAGE 71Ga 0.55±0.05 ・ GALLEX+GNO 71Ga 0.55±0.05 ・ Super-K e- (water) 0.465±0.016 ・ SNO (CC) d (D2O) 0.348±0.020 ・ SNO (NC) d (D2O) 1.01±0.13 B.T.Cleveland et al., Astrophys. J 496 (1998) 505 J.N.Abdurashitov et al., Nucl. Phys. Proc. Suppl. (Neutrino 2002) 118 (2003) 39 T.A.Kirsten for the GNO collab. Nucl. Phys. Proc. Suppl. (Neutrino 2002) 118 (2003) 33. S.Fukuda et al., Phys. Lett. B 539 (2002) 179. Q.R. Ahmad et al., Phys. Rev. Lett. 89 (2002) 011301 http://www.sns.ias.edu/~jnb/

  17. R.Davis Jr. at Homestake Radiochemical solar neutrino experiment 1st prenatal move Solar neutrino deficit; Only 1/3 of the theoretically expected flux. R.Davis Jr., D.S.Harmer and K.C.Hoffman, Phys. Rev. Lett. 20 (1968) 1205. B.T.Cleveland et al., Astrophys. J. 496 (1998) 505.

  18. Homestake solar neutrino experiment ne+Cl37 to e-+Ar37 And then observe the decay of Ar37. Arrival Direction: No. Arrival Time: 1 month. Energy spectrum: No.

  19. L.Wolfenstein, A.Yu Smirnov and S.P.Mikheyev Enhancement of ne oscillation in e-rich media. ( This mechanism effective for zero mass neutrinos, however, turned out not to be necessary. The neutrinos do have non-zero masses and they oscillate among themselves.) S,P.Mikheyev and A.Yu.Smirnov, Sov. J. Nucl. Phys.42 (1985) 1441. L.Wolfenstein, Phys. Rev.D 17 (1978) 2369.

  20. The astrophysical observation. • The astrophysical observation, i.e., with time T, arrival direction D and energy spectrum E, of the solar neutrinos was made by observing the Cherenkov light emitted in the water by the electron struck by these solar neutrino. • KamiokaNDE of 3000tons of water was for the feasibility experiment of the astrophysical observation of the solar neutrinos. • Super-KamiokaNDE was built as the genuine solar neutrino observatory.

  21. KamiokaNDE with 20”f photomultipliers

  22. The KamiokaNDE performance at the beginning of 1987.

  23. Supernova 1987A in the Large Magellanic Cloud. Above; before the explosion. Below; after the explosion.

  24. 2nd prenatal move The observed signal of the supernova neutrino burst. It was immediately confirmed by IMB experiment in USA. The combined results, Tnof 4.5MeV and the total n energy output of 3x1053erg gave strong supports to the theoretical model. The pulse duration of 10msec implies the pre-neutron star density for emmitting these neutrinos. But no directional information.

  25. Creation ofthe 92 chemical elements. • Soon after the Big-Bang, protons and neutrons were created and thus Hydrogen and Helium nuclei with a very minute amount of Lithium. • Heavier nuclei up to Fe were synthesized inside of large stars. • In the Type-II supernova explosion, a large number of neutrons are liberated and they stick to the existing nuclei to form up to U nuclei. All these nuclei are spread out by the explosion into the space and they serve as the material for forming next generation stars. • The sun and the earth are of this late generation. • Now all the 92 chemical elements are available for creating us human being. The neutrinos made this explosion possible by carrying more than 99.9% of the gravitational energy. We should deeply thank the neutrinos!

  26. KamiokaNDE (1st 450 days) K.S.Hirata et al., Phys. Rev. Lett. 63 (1989) 16. Directional observation, D, of the solar neutrinos. Timing, T, is better than 10 ns. Energy spectrum, E, was also observed. See the next slide.

  27. Birth of Neutrino Astrophysics The observed energy spectra of the recoil electrons. It is consistent with the spectra expected from the B8 neutrinos. The intensity, however, is only about a half of that expected from the theory. The solar neutrino anomaly discovered by R.Davis’s radio-chemical experiment was confirmed.

  28. nm/ne has to be 2 or larger Look at the ratio of the upward-going events

  29. m/e ratio measurements Y.Fukuda et al., Phys. Lett. B 335 (1994) 237 R. Becker-Szendy et al., Phys. Rev. D 46 (1992) 3720. R.Clark et al., Phys. Rev. Lett. 79 (1997) 345. M.Aglietta et al., Europhys. Lett. 8 (1989) 611. K.Daum et al., Z. Phys. C 66 (1995) 417. M.Sanchez et al., Phys. Rev. D 68 (2003) 113004 Y. Ashie et al. (Super-Kamiokande collaboration), draft in Preparation.

  30. Neutrino Oscillation • From the observed anomaly in the atmospheric neutrino fluxes, KamiokaNDE concluded that nms produced originally are transforming in flight into nts.

  31. Super-KamiokaNDE, 50ktons H2O, 11,500PMTs

  32. Display of the inner wall of Super-KamiokaNDE A m has just entered the detector.

  33. 50nsec later： Cerenkov light proceeds. Red dots indicate the PMTs of large number of photons received.

  34. The m has reached to the bottom of the detector, while the Cerenkov light in water is still on its way.

  35. Cerenkov light also reached the bottom.

  36. We now see the entire Cerenkov light pattern.

  37. The top e-event has a blurred radial distribution of Cerenkov photons, while the bottom m-event has a crisp ring image. The discrimination between e and mis accomplished by the quantitative comparison of the radial distributions; with a misidentification probability of less than 1%. Note that the m-event has the decay electron later.

  38. Directional Solar n signal above 5 MeV .465 of the theoretically expected flux Super-KamiokaNDE S.Fukuda et al., Phys. Lett. B 539 (2002) 179. 1496days

  39. The observed electron energy spectrum compared to that expected for the B8 decay neutrinos Super-KamiokaNDE M.Smy, et al., Phys. Rev. D 69 (2004) 011104

  40. Super-KamiokaNDE and SNO (2001)The final answer to the solar neutrino deficit Q.R.Ahmad et al., Phys. Rev. Lett. 87 (2001) 071301.

  41. Mixing parameters of Solar neutrino oscillation M.Smy, et al., Phys. Rev. D 69 (2004) 011104 Q.R. Ahmad et al., Phys. Rev. Lett. 89 (2002) 011301 SSM flux independent

  42. Neutrino Oscillation from Zenith angle distributions 1489day FC+PC data + 1646day upward going muon data No osc. Y.Ashie et al., draft in preparation. E.Kearns, for the SK collaboration, talk at Neutrino 2004. Osc.

  43. 1489 days FC+PC (Super-K) Y.Ashie et al., SK collab. hep-ex/0404034 Neutrino Oscillation by L/E analysis (1) Mostly up-going Best fit expectation w/ systematic errors MC (no osc.) Mostly down-going First dip is observed as expected from neutrino oscillation

  44. Allowed regions for nm to ntoscillation 90% CL Soudan2 SK L/E analysis K2K MACRO SK Zenith angle analysis M.Sanchez et al., Phys. Rev. D 68 (2003) 113004 M.Ambrosio et al., Phys. Lett. B 566 (2003) 35. T.Nakaya (for the K2K collaboration), presented at Neutrino2004. Y.Ashie et al., hep-ex/0404034 Y.Ashie et al., draft in preparation; E.Keanrs, for the SK collaboration, talk at Neutrino2004.

  45. electronicshut ＫａｍＬＡＮＤ SK control room N2generator water purification KamLAND liquid scintillator purification

  46. New KamLAND results.(anti-ne behaves the same as ne) 766 ton・year exposure T.Araki et al., hep-ex/0406035 Energy spectrum L/E distribution

  47. K2K(Accerator Neutrino Oscillation Experiment) 250km Neutrino oscillation probability for Δm2=0.003eV2 and at 250km. Eν(GeV)

  48. Now What? • 3 neutrino mixing is established and all the mixing parameters, except the 1-3 mixing angle, are determined. The planned experiment at Gran-Sasso or the future T2K experiment will complete the information. • KamLAND observed the anti-ne from inside the earth. Now the anti-ve tomography is feasible for U,Th and K deposits in the earth core; using several KamLAND type detectors . • The observation of Cosmic Neutrino Background to infer the state of Universe 3 seconds after Big-Bang is indeed still remainig extremely difficult.

  49. Thank you for your patience M. Koshiba

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