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RUNJOB and related topics

RUNJOB and related topics. Toru Shibata INFN, Milano (Aoyama-Gakuin University) 09/September/’04. Contents :. 1) RUNJOB performance. 2) Procedure in RUNJOB data analysis. => Astrop. Phys. 16 (2001) 13, Apanasenko A.V. et. al. 3) RUNJOB results and comparison with other data.

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RUNJOB and related topics

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  1. RUNJOB and related topics Toru Shibata INFN, Milano (Aoyama-Gakuin University) 09/September/’04

  2. Contents : 1) RUNJOB performance 2) Procedure in RUNJOB data analysis => Astrop. Phys. 16 (2001) 13, Apanasenko A.V. et. al. 3) RUNJOB results and comparison with other data 4) Theoretical implication of the experimental data

  3. RUNJOB RUssia-Nippon JOint Balloon experiment M.Furukawa, V.I. Galkin, M. Hareyama, Y. Hirakawa, M. Ichimura, N. Inoue, E. Kamioka, T. Kobayashi, V.V. Kopenkin, S. Kuramata, A.K. Managadze, H. Matsutani, N.P. Misnikova, R.A. Mukhamedshin, S. Nagasawa, R. Nakano, M. Namiki, M. Nakazawa, H. Nanjo, S.N. Nazarov, S. Ohata,H. Ohtomo, D.S. Oshuev, P.A. Publichenko, I.V. Rakobolskaya,T.M. Roganova, C. Saito, G.P. Sazhina, H. Semba, T. Shibata, D. Shuto, H. Sugimoto, R. Suzuki, L.G. Sveshnikova, R.Tanaka, V.M. Taran,N. Yajima, T. Yamagami, I.V. Yashin, E.A. Zamchalova, G.T. Zatsepin, I.S. Zayarnaya Faculty of Engineering, Aomori University, Aomori 030-0943, Japan Department of Physics, Aoyama Gakuin University, Tokyo 157-8572, Japan Faculty of Science and Technology, Hirosaki University, Hirosaki 036-8561, Japan School of Medicine, Hirosaki University, Hirosaki 036-8562, Japan P.N.Lebedev Physical Institute of Russian Academy of Sciences, Moscow 117924, Russia Physical Department of Moscow State University, Moscow 119899, Russia D.V.Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow 119899, Russia Institute for Nuclear Researches of Russian Academy of Sciences, Moscow 117312, Russia Multimedia Information Research Division, National Institute of Informatics The Ministry of Education, Tokyo 101-8430, Japan Shonan Institute of Technology, Fujisawa 251-8511, Japan Department of Management, Urawa University, Urawa 337-0974, Japan

  4. launching mid. July level flight at 32km exp. time ～ 150hrs recovery dismounting early August process. mid. Aug. Performance of RUNJOB experiments construction early May (ISAS, ICRR)

  5. Balloon Trajectory landing launching

  6. Balloon Altitude RUNJOB1,2 RUNJOB3,4 RUNJOB8,9 RUNJOB10,11 Average altitude ~ 32km ~ 10g/cm2

  7. RUNJOB detector target (～10cm) spacer (～20cm) thin EC(～5c.u.) diffuser (～4cm)

  8. Procedure in RUNJOB data analysis: 1) Energy determination 2) Charge determination 3) Detection efficiency calculation RUNJOB results and comparison with other data: 1) Light elements (p, He) 2) Heavy elements (CNO, NeMgSi, Fe) 3) 2-ry/1-ry ratio (B/C, sub-Fe/Fe) 4) All-particle spectrum and average mass

  9. （Moscow04)

  10. (Moscow04)

  11. (summarized by V. Zatsepin)

  12. Summary on RUNJOB data (1) ･95% of all data was analyzed. ･The spectra cover the energy range 10 -1000 TeV for proton 5 - 100 TeV/n for helium 1 - 70 TeV/n for CNO 1 - 20 TeV/n for NeMgSi 0.5 - 8 TeV/n for iron ･Proton spectrum doesn’t’ show any tendency of steeping in observed energy range. ･Helium flux is lower (about half) than JACEE , SOKOL ATIC, but consistent with MUBEE and Grigorov data. ･Proton and helium spectra are nearly parallel

  13. Summary on RUNJOB data (2) ・CNO spectrum has no indication of enhancement in > 10TeV/n region. ・Iron spectrum is consistent with other groups within statistical error ・2-ry/1-ry ratio was shown in TeV/n region. ・All particle spectrum and average mass covers the energy range from 30 to 1000TeV/particle. ・All particle flux is lower than other direct measurement, but seems to be consistent with ATIC (Moscow04) ・The Spectrum shape is similar to other direct measurement => flattering before knee ? ・Average mass is nearly constant in our observation region, 30-1000 TeV with <ln A> ~1.5 (helium)

  14. Procedure in RUNJOB data analysis: 1) Energy determination 2) Charge determination 3) Detection efficiency calculation RUNJOB results and comparison with other data: 1) Light elements (p, He) 2) Heavy elements (CNO, NeMgSi, Fe) 3) 2-ry/1-ry ratio (B/C, sub-Fe/Fe) 4) All-particle spectrum and average mass Theoretical implication of the experimental data: 0) Motivation 1) Model of CR propagation 2) 2-ry/1-ry ratio, isotope, diffusiveγ-ray, anti-p, ……

  15. Present status of C.R. direct obs. in GeV-PeV region observables:physics: ◎1-ry nuclei (p, He, ….., Fe): accel. limit, source spectrum ◎2-ry nuclei (LiBeB, sub-Fe) : path length, residence time - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - ◎ultra-heavy nuclei : r-process, s-process ◎anti-particle (p, e+, ……): novel source, path length ◎isotopes (Be10, Al26, Cl36, …) : life time of C.R., gas density ◎electrons : nearby source, anisotropy ◎diffusive γ-rays: gas density, novel source in harmony with each other ?  if not, novel source ?

  16. Configuration of our Galaxy

  17. r |z| →∞ →∞ Our model ● gas density : ● diff. coefficient : with ● CR source density : with ● boundaryless Galaxy :

  18. Important parameters: ： ● ～ : Kraichnan - type ● : Kolmogorov- type : : ● :

  19. ν= 1 [1 + zDzn] ～zn/zD(～0.1) Practically, we presume zD≫zn (thin gas disk surrounded by a large diffusion space)

  20. 1) primary component: 2) secondary component 0) structure function: <= ApJ, Vol. 612 (Sep. , 2004), Shibata et. al.

  21. Comparison with experimental data : 0）Cosmic-ray data on 1-ry, and 2-ry/1-ry ratio 1） Cosmic-ray data on 10Be/9Be ratio 2）Longitudinal distribution (EGRET & COS-B) 3）Latitudinal distribution (EGRET) 4）Energy distribution in GeV region (EGRET) 5）Energy distribution in TeV (ground-base)

  22. ( average path length) ● at : gas density at Galactic center for : scale height of diffusion coeffi.

  23. (preliminary)

  24. ● τ at ｙ : life time of 10Be for τ : scale height of diffusion coeffi.

  25. Comparison with experimental data : 0）Cosmic-ray data on 1-ry, and 2-ry/1-ry ratio 1） Cosmic-ray data on 10Be/9Be ratio 2）Longitudinal distribution (EGRET & COS-B) 3）Latitudinal distribution (EGRET) 4）Energy distribution in GeV region (EGRET) 5）Energy distribution in TeV (ground-base)

  26. ApJ, vol. 612 (‘04, sep.) 3)γ-ray component z line of sight γ 0 y L l b Earth x

  27. ① E0~1 GeV：　　Bugg et al. (1964) ②10 ~ 300GeV：　　Jaeger et al. (1975) ③400 ~ 2000GeV：　　Neuhofer et al. (1972) ④30~700 TeV ：　　Chacaltaya (1980) , (UA7)

  28. (in CMS)

  29. <= isotropic dist. in CMS

  30. only relative value is compared !

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