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チャカルタヤ山宇宙線共同実験

チャカルタヤ山宇宙線共同実験. 玉田雅宣　（近畿大学） 本田　建　（山梨大学） 他Ｃｈａｃａｌｔａｙａ　Ｃｏｌｌａｂｏｒａｔｏｒ. Collaborator. M.Tamada 5 ,K.Honda 1 ,N.Ohmori 3 ,K.Shinozaki 4 ,N.Inoue 4 ,N.Kawasumi 2 ,N.Ochi, K.Hashimoto 2 ,I.Tsushima 2 ,A.Ohsawa 6 ,H.Aoki 7 ,K.Yokoi 8 ,T.Matano 9 , N.Martinic 10 ,R.Ticona 10 ,C.Aguirre 10

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チャカルタヤ山宇宙線共同実験

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  1. チャカルタヤ山宇宙線共同実験 玉田雅宣　（近畿大学） 本田　建　（山梨大学） 他Ｃｈａｃａｌｔａｙａ　Ｃｏｌｌａｂｏｒａｔｏｒ

  2. Collaborator M.Tamada5 ,K.Honda1,N.Ohmori3,K.Shinozaki4,N.Inoue4,N.Kawasumi2,N.Ochi, K.Hashimoto2,I.Tsushima2,A.Ohsawa6,H.Aoki7,K.Yokoi8,T.Matano9, N.Martinic10,R.Ticona10,C.Aguirre10 [1]Faculty of Engineering, Yamanashi University, Kofu, 400-8511, Japan[2]Faculty of Education, Yamanashi University, Kofu,400-8510, Japan[3]Faculty of Science, Kochi University, 780-8520, Japan[4]Faculty of Science, Saitama University, 388-8570, Japan[5]Faculty of Science and Technology, Kinki University, 577-8520, Japan[6]Institute for Cosmic Ray Research, University Tokyo, 277-8582, Japan[7]Faculty of Science, Souka University, 192-8577, Japan[8]College of science and Engineering, Aoyama Gakuin University, 157-8572, Japan[9]Shibakubo-cho 3-28-10,Tanashi,188-0014 Japan[10]Institute de Investigaciones Fisicas Universidad Mayor de San Andres, Bolivia

  3. ? ?

  4. atmospheric family Eg, Rg Eh(g), Rh atmospheric family (A-jets)

  5. Family intensity †proton dominant model [ p(42%),He(17%),CNO(14%),heavy(14%),Fe(13%) at E0=1015eV] †all particles spectrum = EAS data (Tibet, Akeno) QGSJET with EAS sp. gives 3~4 times larger intensity. Violent energy dissipation !?

  6. QGSJET with RUNJOB sp. describes well. †proton dominant model [ p(42%),He(17%),CNO(14%),heavy(14%),Fe(13%) at E0=1015eV] †all particles spectrum = RUNJOB data

  7. Hybrid experiment Air-shower array + Emulsion chamber

  8. Chacaltaya hybrid experiment(Chacaltaya,5200m) 8m2 10m Hadron Calorimeter EAS-array

  9. hadron component in EAS KASCADE T.Antoni et al. J.Phys.G27(2001) 1785, CERN COURIER 42-6(2002) Chacaltaya ESarray+EM ; A.Aguirre et al. PRD62(2000)032003 Models fail to describe hadron number in EAS. strong violation of Feynman scaling law !?

  10. HADRON-M(Tien-Shan, 3340m) 10m Emulsion chamber EAS-array

  11. Tibet ASg(Yangbajing, 4300m) AS-array Emulsion chamber Burst detector

  12. EAS triggered family violent energy dissipation Strong violation of Feynman scaling law at E0≥1016eV !?

  13. Discrepancy is due to statistical fluctuation ?? All particles : Tibet > RUNJOB Protons, He : Tibet ~ RUNJOB Heavy : Tibet > RUNJOB Tibet data Tibet : PRD62(2000)112002 Proc. ICRC2001,148 Fe(Tibet HD-model) Proton(Tibet HD-model) RUNJOB: Astrop. Phys.16(2001) 13

  14. Cosmic-ray nuclear interaction at E0=1015~1017eV is still far from full understanding. • Changes of primary composition alone solve the discrepancies between experimental data and model prediction (Tibet group) ?? • There seems no possibility. Changes of nuclear interaction are necessary. Severe energy dissipation etc. (Strong vilation of Feynman Scaling law) Role of exotics ?

  15. 1013 1014 1015 1016 1017 1018 1019 1020 Tevatron LHC SppS E0 (eV) emulsion chamber + Air Shower array emulsion chamber Air Shower array C-jets families ‘halo’ families with EAS data EAS beyond GKZ unexplained (exotic) events mild violation of Feynman scaling law strong violation of Feynman scaling law ? QGSJET OK !! QGSJET OK ??? ?

  16. future prospect ATHLET

  17. measurement of emulsion chamber data is very time consuming semi-automatic measurement using image-scanner ; successful in Tibet group, (Nucl. Instr. Meth. A523(2004) 193) in progress in Chacaltaya group & Pamir group

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