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C osmic-rays and Particle physics

C osmic-rays and Particle physics. (based on Brazil-Japan Emulsion Collaboration). Toru Shibata. Aoyama- Gakuin University 17/Aug/2010. April 12, 1912. l a ~ cm. *. l b ~ m. *. l g ~ 10 m. * . r adiation from space !!!. 1933: (Alvarez)

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C osmic-rays and Particle physics

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  1. Cosmic-rays and Particle physics (based on Brazil-Japan Emulsion Collaboration) Toru Shibata Aoyama-Gakuin University 17/Aug/2010

  2. April 12, 1912 la ~ cm * lb ~ m * lg~ 10 m * radiation from space !!! 1933: (Alvarez) east-west asymmetry effect positive charged particle !

  3. cosmic rays magnetic field

  4. q E W SANRIKU (b, l) = (39.2。N, 141.8。E) : our data histogram: simulation Astrop. Phys. 6 (1997) 155 E W

  5. Astrop. Phys. 6 (1997) 155 filled symbols: E-W effect method open symbols: opening-angle method

  6. age of new particles: 1930~1950 1932: positron (Anderson) Dirac Theory 1935: Yukawa hypothesis 1937: m-meson (Anderson & Neddermyer) 1947: p-meson (Lattes, Ochiallini, & Powell) Yukawa Theory (birth of elementary particle physics) 1947: V-particle (Rochester & Butler) strangeness Sakata, Gell-Mann quark model 1948: p-meson with machine (Gardner & Lattes)

  7. cosmic-ray physics after 1950 1-ry CRs 1-ry CRs astrophysics 2-ry CRs 2-ry CRs particle phys. big machine

  8. definitionof“cosmic rays” ●nuclei (p, He, ….., Fe, …) : in narrow sense particle astronomy ●　antiparticles (p, He, …) : ●　electrons & positrons : ●　neutrinos : in wide sense (neutrino astronomy) g-ray astronomy ●　g-rays : ●X-rays : in wider sense X-ray astronomy ultraviolet-visible-infrared-radio : related field astronomy infrared astronomy radio astronomy

  9. I. Cosmic-rays and Particle physics after 1950 new particle search“big” machine go to higher energy (>> machine energy ~ GeV) >TeV multiple meson production key to solve difficulty in Field Theory ? Heisenberg: universal length (1939) Wataghin: cutoff momentum (19??) => fireball production Fermi, Landau: thermo-statistical model (1950, 1953) Miesowicze, Cocconi, Niu, Hasegawa: two fireball (1958), H-q.(1961) . . . . . . . .

  10. ICRC International Cosmic Ray Conference 1947: 1st ICRC @ Cracow,Poland 2013: 33th ICRC @ Rio de J., Brazil 2014: World cup @ Rio de Janeiro, Brazil !!! 2016: Olympiad @ Rio de Janeiro, Brazil !!!

  11. sessions in ICRC HE: High Energy Interactions EA: Air shower phenomena MN: Muon, Nutrino OG: Origin of CRs SH: Solar Heliosphere T: Techniques

  12. short history of emulsion chamber in CR research 1952: Emulsion stack => new particle hunting (Bristol) => but poor cost-effectiveness Brass plate emulsion chamber (EC) => A-dependence (Rochester) 1955: EC project starts in INS (Inst. of Nuclear Study, University of Tokyo) Balloon exposure with baby EC (Kobe-group) (Fujimoto comes back from Bristol) E0=1~10TeV 1956: Balloon flight => pt-invariance (Nishimura) 1958: EC exposure at Mt. Norikura => g, hadron spectra 10~100TeV => g, hadron bundle 1959: Letter of Yukawa to Lattes 1962: Brazil-Japan collaboration at Mt. Chacaltaya First exposure of simple-type EC > 1000TeV ~

  13. basic structure of EC _ + shower curve (1987, NIM-A257) hadron(p, n, p) e-, g Pb-jet EM-cascade shower e -, g + Pb => bremsstrahlung, pair-creation => EM cascade shower p +’s hadron+ Pb + p -’s + p 0’s p0 2g EM cascade shower

  14. for Balloon experiment 1 1-ry layer : target layer : 2 spacer : calorimeter : (EC) 3 4 cascade p0 2g

  15. Physics in emulsion chamber _ + ●accelerator: neutrino oscillation (nm nt; OPERA) composition of CRs=> origin, accle., prop. ; anomalies in [e , p] => signal of DM, PBH ? ; ●balloon: exotics => q-nugget, mono-pole . . . ? ●high mountain: forwardhadron physics => nothing new in small q2 ? => very difficult to see with machine (important for the EAS study) LHC

  16. ECs used in Brazil-Japan collaboration 2-types of EC local interaction (C-jet) atmospheric int. (A-jet) “clean” “dirty” H＝100 ~ 1000m target p+’s p-’s p 0’s H＝1 ~ 2m p0 2g r ~ 1mm r ~ 10cm EC

  17. number of pairs per 30MeV/c2

  18. Physics in Brazil-Japan collaboration personal speculation similarity in multiple meson production H-quantum Feynman-scaling C-jet : d3pg F(E0 ;Eg, pt) = f(x)dx g(pt)2pptdpt Eg with x = Eg/E0 E0 deviation from pt-invariance SH-quantum (break in Feynman-scaling) production cross-sections of g ’s in p-p collision in very forward region ten years earlier than CERN-SPS pt = pgsinq (Eg, pt)i (i=1, . . ,n) (p 0 2g )

  19. A-jet : extremely massive fire-ball with high temperature UH-quantum H-quantum SH-quantum UH-quantum Mass: 1 ~ 2GeV/c2 10 ~ 20GeV/c2 100 ~ 200GeV/c2 < pt>: ~0.3 GeV/c ~0.5 GeV/c ~1.0 GeV/c (temperature) “new state of matter” (H-q, SH-q, UH-q) discovery of “ANDROMEDA” air shower core just before cascade development Exotics: CENTAURO, Geminion, CHIRON, . . .

  20. fireball physics in BJ-collaboration before collision N N X critical parameters: in CMS fireball mass M after collision fireball temperature T (both are quantized) “new state of matter” ? phenomenological stage substantialistic stage essentialistic stage Taketani’s three-stage theory in cognition of nature

  21. Statistical mechanics Quantummechanics Thermodynamics (substantialistic stage ?) (essentialistic stage ?)

  22. 1977: R. D. Field and R. P. Feynman, Phys. Rev. D15, 2590 1978: R. P. Feynman, R. D. Field, and G. C. Fox, Phys. Rev. D18, 3320 (1969: “Parton” model by Feynman for SLAC e-p deep inelastic data) ! proton electron parton 1 s = 2

  23. mechanism of multiple meson production (based on “parton” model) (a) lepton-hadron (c) hadron-hadron (b) lepton-lepton

  24. break in pt-invariance in fireball picture break in pt-invariance in “parton” picture H-q -6pt -6pt d3s d3s e e E E d3p d3p : pt-invariance SH-q signal of point-point int. Rutherford scattering UH-q pt(GeV/c) pt(GeV/c)

  25. questions in hadron-hadron collision: (e) (e) (e) (e) q q q q g g (g ) (g ) q q q q (e) (e) (e) (e) (Mfller scattering) (Rutherford scattering !!) ??? ISR data

  26. Why not pT-4, but pT-8? “-8” => many models modifying point-point interaction approach not “essential”, but “acceidental” due to QCD effect (Feynman et al. 1978, Phys. Rev.) not yet asymptotic free in the data available higher order corrections for point-point int. g - q g q q

  27. : Feynman variable : fractional g-ray energy E0 pt = pgsinq (Eg, pt)i (i=1, . . ,n) (p 0 2g )

  28. E0 1TeV (ISR) E0 100TeV (B-J)

  29. 1978: Feynman et al., Phys. Rev. D18, 3320 central region (covered by machine) CMS backward forward (covered by EC) our target central region

  30. 1980, Phys. Rev. D22, 100

  31. large pt phenomena: We, CR physicists, have already observed point-point interactions in hadron-hadron collisions in the form of large pt-phenomena!! 1962: M. Oda and Y. Tanaka, J. Phys. Soc. Jpn. 17, Suppl. A-III, 282 1963: S. Miyake, K. Hinotani, and T. Kaneko, J. Phys. Soc. Jpn. 18, 592 multi-cores in air shower observation (far from “normal” pt with ~ 300 MeV/c => heavy 1-ry) 1967: Brazil-Japan Collaboration, Canadian J. Phys. 46, 660 first two-storey-type emulsion chamber (interpreted as H-, SH-quanta productions)

  32. “parton” = quarks, gluons 1990: Nobel prize for Friedman, Kendall, Tayler (MIT-SLAC) We missed a signal of “parton” in CR data much earlier than MIT-SLAC !!!

  33. Exotics : CENTAURO, Geminion, CHIRON, . . . I could not follow these “ZOO-series” , whileI have learned many things from Profs. Lattes, Fujimoto, and Hasegawa I moved to 1-ry CR study with balloon

  34. (Letter of Prof. Y. Fujimoto to Colleague; 28/Oct/1998)

  35. Thank you

  36. Illustration of CENTAURO I

  37. production cross-sections of g ’s in p-p collision in very forward region ten years earlier than CERN-SPS H.E. EAS study key data for g-ray astronomy p p E0 before collision : Eg ’ E0 X after collision : proton + proton g+ anything s(E0 ,Eg)dEg

  38. Astrop. Phys. 23(2005)510 due to detection bias

  39. (compiled by Stecker)

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