Heavy component spectra and secondary to primary ratios obtained by RUNJOB experiment

M. Ichimura; V. A. Derbina; V. I. Galkin; M. Hareyama; Y. Hirakawa; Y. Horiuchi; 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; V. I. Osedlo; 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; V. M. Taran; N. Yajima; T. Yamagami; I. V. Yashin; E. A. Zamchalova; G. T. Zatsepin; I. S. Zayarnaya

Heavy component spectra and secondary to primary ratios obtained by RUNJOB experiment

M. Ichimura, V. A. Derbina, V. I. Galkin, M. Hareyama, Y. Hirakawa, Y. Horiuchi, 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. NanjoS. N. Nazarov, S. Ohata, H. Ohtomo, V. I. Osedlo, 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, V. M. Taran, N. Yajima, T. Yamagami, I. V. Yashin, E. A. Zamchalova, G. T. Zatsepin, I. S. Zayarnaya

研究成果 › 査読

3 被引用数 (Scopus)

抄録

RUNJOB final results on the energy spectra of primary heavy cosmic ray components are presented. Data are from ten RUNJOB campaigns performed from 1995 through 1999. And the energy spectra of CNO, NeMgSi and Fe groups are shown here as well as the energy dependence of the secondary/primary ratio. We find our heavy component spectra are in agreement with the extrapolation from those at lower energies obtained by CRN (Chicago group), monotonically decreasing with energy, in contrast to JACEE and SOKOL data, which indicated a gradual increase with energy, particularly for the CNO group at ̃ 5 TeV/nucleon. As for the secondary to primary ratio we have observed in TeV/nucleon energy region, it is difficult to determine the energy dependence of their average path lengths by the RUNJOB data only, because the large uncertainty of atmospheric corrections due to the poor statistics exists.

本文言語	English
ページ	21-24
ページ数	4
出版ステータス	Published - 2005
外部発表	はい
イベント	29th International Cosmic Ray Conference, ICRC 2005 - Pune, India 継続期間: 2005 8月 3 → 2005 8月 10

Conference

Conference	29th International Cosmic Ray Conference, ICRC 2005
国/地域	India
City	Pune
Period	05/8/3 → 05/8/10

ASJC Scopus subject areas

核物理学および高エネルギー物理学

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引用スタイル

Ichimura, M., Derbina, V. A., Galkin, V. I., Hareyama, M., Hirakawa, Y., Horiuchi, Y., Inoue, N., Kamioka, E., Kobayashi, T., Kopenkin, V. V., Kuramata, S., Managadze, A. K., Matsutani, H., Misnikova, N. P., Mukhamedshin, R. A., Nagasawa, S., Nakano, R., Namiki, M., Nakazawa, M., ... Zayarnaya, I. S. (2005). Heavy component spectra and secondary to primary ratios obtained by RUNJOB experiment. 21-24. Paper presented at 29th International Cosmic Ray Conference, ICRC 2005, Pune, India.

Ichimura, M, Derbina, VA, Galkin, VI, Hareyama, M, Hirakawa, Y, Horiuchi, Y, Inoue, N, Kamioka, E, Kobayashi, T, Kopenkin, VV, Kuramata, S, Managadze, AK, Matsutani, H, Misnikova, NP, Mukhamedshin, RA, Nagasawa, S, Nakano, R, Namiki, M, Nakazawa, M, Nanjo, H, Nazarov, SN, Ohata, S, Ohtomo, H, Osedlo, VI, Oshuev, DS, Publichenko, PA, Rakobolskaya, IV, Roganova, TM, Saito, C, Sazhina, GP, Semba, H, Shibata, T, Shuto, D, Sugimoto, H, Suzuki, R, Sveshnikova, LG, Taran, VM, Yajima, N, Yamagami, T, Yashin, IV, Zamchalova, EA, Zatsepin, GT & Zayarnaya, IS 2005, 'Heavy component spectra and secondary to primary ratios obtained by RUNJOB experiment', Paper presented at 29th International Cosmic Ray Conference, ICRC 2005, Pune, India, 05/8/3 - 05/8/10 pp. 21-24.

@conference{6d6fb937071441ffbb3b1eacf1b41010,

title = "Heavy component spectra and secondary to primary ratios obtained by RUNJOB experiment",

abstract = "RUNJOB final results on the energy spectra of primary heavy cosmic ray components are presented. Data are from ten RUNJOB campaigns performed from 1995 through 1999. And the energy spectra of CNO, NeMgSi and Fe groups are shown here as well as the energy dependence of the secondary/primary ratio. We find our heavy component spectra are in agreement with the extrapolation from those at lower energies obtained by CRN (Chicago group), monotonically decreasing with energy, in contrast to JACEE and SOKOL data, which indicated a gradual increase with energy, particularly for the CNO group at{\~ } 5 TeV/nucleon. As for the secondary to primary ratio we have observed in TeV/nucleon energy region, it is difficult to determine the energy dependence of their average path lengths by the RUNJOB data only, because the large uncertainty of atmospheric corrections due to the poor statistics exists.",

author = "M. Ichimura and Derbina, {V. A.} and Galkin, {V. I.} and M. Hareyama and Y. Hirakawa and Y. Horiuchi and N. Inoue and E. Kamioka and T. Kobayashi and Kopenkin, {V. V.} and S. Kuramata and Managadze, {A. K.} and H. Matsutani and Misnikova, {N. P.} and Mukhamedshin, {R. A.} and S. Nagasawa and R. Nakano and M. Namiki and M. Nakazawa and H. Nanjo and Nazarov, {S. N.} and S. Ohata and H. Ohtomo and Osedlo, {V. I.} and Oshuev, {D. S.} and Publichenko, {P. A.} and Rakobolskaya, {I. V.} and Roganova, {T. M.} and C. Saito and Sazhina, {G. P.} and H. Semba and T. Shibata and D. Shuto and H. Sugimoto and R. Suzuki and Sveshnikova, {L. G.} and Taran, {V. M.} and N. Yajima and T. Yamagami and Yashin, {I. V.} and Zamchalova, {E. A.} and Zatsepin, {G. T.} and Zayarnaya, {I. S.}",

year = "2005",

language = "English",

pages = "21--24",

note = "29th International Cosmic Ray Conference, ICRC 2005 ; Conference date: 03-08-2005 Through 10-08-2005",

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TY - CONF

T1 - Heavy component spectra and secondary to primary ratios obtained by RUNJOB experiment

AU - Ichimura, M.

AU - Derbina, V. A.

AU - Galkin, V. I.

AU - Hareyama, M.

AU - Hirakawa, Y.

AU - Horiuchi, Y.

AU - Inoue, N.

AU - Kamioka, E.

AU - Kobayashi, T.

AU - Kopenkin, V. V.

AU - Kuramata, S.

AU - Managadze, A. K.

AU - Matsutani, H.

AU - Misnikova, N. P.

AU - Mukhamedshin, R. A.

AU - Nagasawa, S.

AU - Nakano, R.

AU - Namiki, M.

AU - Nakazawa, M.

AU - Nanjo, H.

AU - Nazarov, S. N.

AU - Ohata, S.

AU - Ohtomo, H.

AU - Osedlo, V. I.

AU - Oshuev, D. S.

AU - Publichenko, P. A.

AU - Rakobolskaya, I. V.

AU - Roganova, T. M.

AU - Saito, C.

AU - Sazhina, G. P.

AU - Semba, H.

AU - Shibata, T.

AU - Shuto, D.

AU - Sugimoto, H.

AU - Suzuki, R.

AU - Sveshnikova, L. G.

AU - Taran, V. M.

AU - Yajima, N.

AU - Yamagami, T.

AU - Yashin, I. V.

AU - Zamchalova, E. A.

AU - Zatsepin, G. T.

AU - Zayarnaya, I. S.

PY - 2005

Y1 - 2005

N2 - RUNJOB final results on the energy spectra of primary heavy cosmic ray components are presented. Data are from ten RUNJOB campaigns performed from 1995 through 1999. And the energy spectra of CNO, NeMgSi and Fe groups are shown here as well as the energy dependence of the secondary/primary ratio. We find our heavy component spectra are in agreement with the extrapolation from those at lower energies obtained by CRN (Chicago group), monotonically decreasing with energy, in contrast to JACEE and SOKOL data, which indicated a gradual increase with energy, particularly for the CNO group at ̃ 5 TeV/nucleon. As for the secondary to primary ratio we have observed in TeV/nucleon energy region, it is difficult to determine the energy dependence of their average path lengths by the RUNJOB data only, because the large uncertainty of atmospheric corrections due to the poor statistics exists.

AB - RUNJOB final results on the energy spectra of primary heavy cosmic ray components are presented. Data are from ten RUNJOB campaigns performed from 1995 through 1999. And the energy spectra of CNO, NeMgSi and Fe groups are shown here as well as the energy dependence of the secondary/primary ratio. We find our heavy component spectra are in agreement with the extrapolation from those at lower energies obtained by CRN (Chicago group), monotonically decreasing with energy, in contrast to JACEE and SOKOL data, which indicated a gradual increase with energy, particularly for the CNO group at ̃ 5 TeV/nucleon. As for the secondary to primary ratio we have observed in TeV/nucleon energy region, it is difficult to determine the energy dependence of their average path lengths by the RUNJOB data only, because the large uncertainty of atmospheric corrections due to the poor statistics exists.

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UR - http://www.scopus.com/inward/citedby.url?scp=84898968477&partnerID=8YFLogxK

M3 - Paper

AN - SCOPUS:84898968477

SP - 21

EP - 24

T2 - 29th International Cosmic Ray Conference, ICRC 2005

Y2 - 3 August 2005 through 10 August 2005

ER -

Heavy component spectra and secondary to primary ratios obtained by RUNJOB experiment

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