Composition and energy spectra of cosmic-ray primaries in the energy range 1013-1015 eV/particle observed by Japanese-Russian joint balloon experiment

A. V. Apanasenko, V. A. Sukhadolskaya, V. A. Derbina, M. Fujii, V. I. Galkine, G. G. Getsov, M. Hareyama, M. Ichimura, S. Ito, Eiji Kamioka, T. Kitami, T. Kobayashi, V. D. Kolesnikov, V. Kopenkin, N. M. Kotunova, S. Kuramata, Y. Kuriyama, V. I. Lapshin, A. K. Managadze, H. MatsutaniH. Mikami, N. P. Misnikova, R. A. Mukhamedshin, M. Namiki, H. Nanjo, S. N. Nazarov, S. I. Nikolsky, T. Ohe, S. Ohta, V. I. Osedlo, D. S. Oshuev, D. M. Podorozhny, P. A. Publichenko, I. V. Rakobolskaya, T. M. Roganova, M. Saito, G. P. Sazhina, H. Semba, Yu N. Shabanova, T. Shibata, H. Sugimoto, L. G. Sveshnikova, K. Takahashi, T. Tsuchiya, V. M. Taran, N. Yajima, T. Yamagami, K. Yamamoto, I. V. Yashin, E. A. Zamchalova, G. T. Zatsepin, I. S. Zayarnaya

Research output: Contribution to journalArticle

158 Citations (Scopus)

Abstract

We report experimental results obtained by the emulsion chambers on board of the long duration balloon. We have been carrying out the trans-Siberian-continental balloon flight since 1995, and the results from 1995 to 1996 experiments are presented here. Total exposure of these two years amounts to 231.5 m2 h at the average altitude of ~32 km. The energy range covers 10-500 TeV for proton-primary, 3-70 TeV/n for helium-primary, and 1-5 TeV/n for Fe-group (Z=26-28), though statistics of heavy components is not yet enough. Our preliminary data show that the spectra of the proton and the helium have nearly the same power indices ~2.80, while those of heavier ones become gradually harder as the mass gets heavier, for instance the index is ~2.70 for CNO-group and ~2.55 for Fe-group. It is remarkable that a very high energy proton with multi-PeV is detected in 1995 experiment, and the estimated flux of this event coincides with a simple extrapolation from the energy spectrum with the power index 2.8 observed in the range 10-500 TeV. It indicates that there is no spectral break at around 100 TeV, in contrast to the maximum energy predicted by the current shock-wave acceleration model. This evidence requires some modification on the acceleration and/or propagation mechanism. Also we present all-particle spectrum and the average primary mass in the energy range 20-1000 TeV/particle. Our preliminary data show no drastic change in mass composition over the wide energy range, at least up to 1 PeV/particle, though the statistics is not yet enough to confirm it concretely. The flight performance and the procedure of the analysis, particularly the energy determination methods and the detection efficiency calculation are also given.

Original languageEnglish
Pages (from-to)13-46
Number of pages34
JournalAstroparticle Physics
Volume16
Issue number1
DOIs
Publication statusPublished - 2001 Oct
Externally publishedYes

Fingerprint

primary cosmic rays
balloons
energy spectra
helium
energy
statistics
balloon flight
flight characteristics
protons
proton energy
emulsions
extrapolation
shock waves
chambers
propagation

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

Cite this

Apanasenko, A. V., Sukhadolskaya, V. A., Derbina, V. A., Fujii, M., Galkine, V. I., Getsov, G. G., ... Zayarnaya, I. S. (2001). Composition and energy spectra of cosmic-ray primaries in the energy range 1013-1015 eV/particle observed by Japanese-Russian joint balloon experiment. Astroparticle Physics, 16(1), 13-46. https://doi.org/10.1016/S0927-6505(00)00163-8

Composition and energy spectra of cosmic-ray primaries in the energy range 1013-1015 eV/particle observed by Japanese-Russian joint balloon experiment. / Apanasenko, A. V.; Sukhadolskaya, V. A.; Derbina, V. A.; Fujii, M.; Galkine, V. I.; Getsov, G. G.; Hareyama, M.; Ichimura, M.; Ito, S.; Kamioka, Eiji; Kitami, T.; Kobayashi, T.; Kolesnikov, V. D.; Kopenkin, V.; Kotunova, N. M.; Kuramata, S.; Kuriyama, Y.; Lapshin, V. I.; Managadze, A. K.; Matsutani, H.; Mikami, H.; Misnikova, N. P.; Mukhamedshin, R. A.; Namiki, M.; Nanjo, H.; Nazarov, S. N.; Nikolsky, S. I.; Ohe, T.; Ohta, S.; Osedlo, V. I.; Oshuev, D. S.; Podorozhny, D. M.; Publichenko, P. A.; Rakobolskaya, I. V.; Roganova, T. M.; Saito, M.; Sazhina, G. P.; Semba, H.; Shabanova, Yu N.; Shibata, T.; Sugimoto, H.; Sveshnikova, L. G.; Takahashi, K.; Tsuchiya, T.; Taran, V. M.; Yajima, N.; Yamagami, T.; Yamamoto, K.; Yashin, I. V.; Zamchalova, E. A.; Zatsepin, G. T.; Zayarnaya, I. S.

In: Astroparticle Physics, Vol. 16, No. 1, 10.2001, p. 13-46.

Research output: Contribution to journalArticle

Apanasenko, AV, Sukhadolskaya, VA, Derbina, VA, Fujii, M, Galkine, VI, Getsov, GG, Hareyama, M, Ichimura, M, Ito, S, Kamioka, E, Kitami, T, Kobayashi, T, Kolesnikov, VD, Kopenkin, V, Kotunova, NM, Kuramata, S, Kuriyama, Y, Lapshin, VI, Managadze, AK, Matsutani, H, Mikami, H, Misnikova, NP, Mukhamedshin, RA, Namiki, M, Nanjo, H, Nazarov, SN, Nikolsky, SI, Ohe, T, Ohta, S, Osedlo, VI, Oshuev, DS, Podorozhny, DM, Publichenko, PA, Rakobolskaya, IV, Roganova, TM, Saito, M, Sazhina, GP, Semba, H, Shabanova, YN, Shibata, T, Sugimoto, H, Sveshnikova, LG, Takahashi, K, Tsuchiya, T, Taran, VM, Yajima, N, Yamagami, T, Yamamoto, K, Yashin, IV, Zamchalova, EA, Zatsepin, GT & Zayarnaya, IS 2001, 'Composition and energy spectra of cosmic-ray primaries in the energy range 1013-1015 eV/particle observed by Japanese-Russian joint balloon experiment', Astroparticle Physics, vol. 16, no. 1, pp. 13-46. https://doi.org/10.1016/S0927-6505(00)00163-8
Apanasenko, A. V. ; Sukhadolskaya, V. A. ; Derbina, V. A. ; Fujii, M. ; Galkine, V. I. ; Getsov, G. G. ; Hareyama, M. ; Ichimura, M. ; Ito, S. ; Kamioka, Eiji ; Kitami, T. ; Kobayashi, T. ; Kolesnikov, V. D. ; Kopenkin, V. ; Kotunova, N. M. ; Kuramata, S. ; Kuriyama, Y. ; Lapshin, V. I. ; Managadze, A. K. ; Matsutani, H. ; Mikami, H. ; Misnikova, N. P. ; Mukhamedshin, R. A. ; Namiki, M. ; Nanjo, H. ; Nazarov, S. N. ; Nikolsky, S. I. ; Ohe, T. ; Ohta, S. ; Osedlo, V. I. ; Oshuev, D. S. ; Podorozhny, D. M. ; Publichenko, P. A. ; Rakobolskaya, I. V. ; Roganova, T. M. ; Saito, M. ; Sazhina, G. P. ; Semba, H. ; Shabanova, Yu N. ; Shibata, T. ; Sugimoto, H. ; Sveshnikova, L. G. ; Takahashi, K. ; Tsuchiya, T. ; Taran, V. M. ; Yajima, N. ; Yamagami, T. ; Yamamoto, K. ; Yashin, I. V. ; Zamchalova, E. A. ; Zatsepin, G. T. ; Zayarnaya, I. S. / Composition and energy spectra of cosmic-ray primaries in the energy range 1013-1015 eV/particle observed by Japanese-Russian joint balloon experiment. In: Astroparticle Physics. 2001 ; Vol. 16, No. 1. pp. 13-46.
@article{ebe28bb7ce4542cf8b048d874269a5b4,
title = "Composition and energy spectra of cosmic-ray primaries in the energy range 1013-1015 eV/particle observed by Japanese-Russian joint balloon experiment",
abstract = "We report experimental results obtained by the emulsion chambers on board of the long duration balloon. We have been carrying out the trans-Siberian-continental balloon flight since 1995, and the results from 1995 to 1996 experiments are presented here. Total exposure of these two years amounts to 231.5 m2 h at the average altitude of ~32 km. The energy range covers 10-500 TeV for proton-primary, 3-70 TeV/n for helium-primary, and 1-5 TeV/n for Fe-group (Z=26-28), though statistics of heavy components is not yet enough. Our preliminary data show that the spectra of the proton and the helium have nearly the same power indices ~2.80, while those of heavier ones become gradually harder as the mass gets heavier, for instance the index is ~2.70 for CNO-group and ~2.55 for Fe-group. It is remarkable that a very high energy proton with multi-PeV is detected in 1995 experiment, and the estimated flux of this event coincides with a simple extrapolation from the energy spectrum with the power index 2.8 observed in the range 10-500 TeV. It indicates that there is no spectral break at around 100 TeV, in contrast to the maximum energy predicted by the current shock-wave acceleration model. This evidence requires some modification on the acceleration and/or propagation mechanism. Also we present all-particle spectrum and the average primary mass in the energy range 20-1000 TeV/particle. Our preliminary data show no drastic change in mass composition over the wide energy range, at least up to 1 PeV/particle, though the statistics is not yet enough to confirm it concretely. The flight performance and the procedure of the analysis, particularly the energy determination methods and the detection efficiency calculation are also given.",
author = "Apanasenko, {A. V.} and Sukhadolskaya, {V. A.} and Derbina, {V. A.} and M. Fujii and Galkine, {V. I.} and Getsov, {G. G.} and M. Hareyama and M. Ichimura and S. Ito and Eiji Kamioka and T. Kitami and T. Kobayashi and Kolesnikov, {V. D.} and V. Kopenkin and Kotunova, {N. M.} and S. Kuramata and Y. Kuriyama and Lapshin, {V. I.} and Managadze, {A. K.} and H. Matsutani and H. Mikami and Misnikova, {N. P.} and Mukhamedshin, {R. A.} and M. Namiki and H. Nanjo and Nazarov, {S. N.} and Nikolsky, {S. I.} and T. Ohe and S. Ohta and Osedlo, {V. I.} and Oshuev, {D. S.} and Podorozhny, {D. M.} and Publichenko, {P. A.} and Rakobolskaya, {I. V.} and Roganova, {T. M.} and M. Saito and Sazhina, {G. P.} and H. Semba and Shabanova, {Yu N.} and T. Shibata and H. Sugimoto and Sveshnikova, {L. G.} and K. Takahashi and T. Tsuchiya and Taran, {V. M.} and N. Yajima and T. Yamagami and K. Yamamoto and Yashin, {I. V.} and Zamchalova, {E. A.} and Zatsepin, {G. T.} and Zayarnaya, {I. S.}",
year = "2001",
month = "10",
doi = "10.1016/S0927-6505(00)00163-8",
language = "English",
volume = "16",
pages = "13--46",
journal = "Astroparticle Physics",
issn = "0927-6505",
publisher = "Elsevier",
number = "1",

}

TY - JOUR

T1 - Composition and energy spectra of cosmic-ray primaries in the energy range 1013-1015 eV/particle observed by Japanese-Russian joint balloon experiment

AU - Apanasenko, A. V.

AU - Sukhadolskaya, V. A.

AU - Derbina, V. A.

AU - Fujii, M.

AU - Galkine, V. I.

AU - Getsov, G. G.

AU - Hareyama, M.

AU - Ichimura, M.

AU - Ito, S.

AU - Kamioka, Eiji

AU - Kitami, T.

AU - Kobayashi, T.

AU - Kolesnikov, V. D.

AU - Kopenkin, V.

AU - Kotunova, N. M.

AU - Kuramata, S.

AU - Kuriyama, Y.

AU - Lapshin, V. I.

AU - Managadze, A. K.

AU - Matsutani, H.

AU - Mikami, H.

AU - Misnikova, N. P.

AU - Mukhamedshin, R. A.

AU - Namiki, M.

AU - Nanjo, H.

AU - Nazarov, S. N.

AU - Nikolsky, S. I.

AU - Ohe, T.

AU - Ohta, S.

AU - Osedlo, V. I.

AU - Oshuev, D. S.

AU - Podorozhny, D. M.

AU - Publichenko, P. A.

AU - Rakobolskaya, I. V.

AU - Roganova, T. M.

AU - Saito, M.

AU - Sazhina, G. P.

AU - Semba, H.

AU - Shabanova, Yu N.

AU - Shibata, T.

AU - Sugimoto, H.

AU - Sveshnikova, L. G.

AU - Takahashi, K.

AU - Tsuchiya, T.

AU - Taran, V. M.

AU - Yajima, N.

AU - Yamagami, T.

AU - Yamamoto, K.

AU - Yashin, I. V.

AU - Zamchalova, E. A.

AU - Zatsepin, G. T.

AU - Zayarnaya, I. S.

PY - 2001/10

Y1 - 2001/10

N2 - We report experimental results obtained by the emulsion chambers on board of the long duration balloon. We have been carrying out the trans-Siberian-continental balloon flight since 1995, and the results from 1995 to 1996 experiments are presented here. Total exposure of these two years amounts to 231.5 m2 h at the average altitude of ~32 km. The energy range covers 10-500 TeV for proton-primary, 3-70 TeV/n for helium-primary, and 1-5 TeV/n for Fe-group (Z=26-28), though statistics of heavy components is not yet enough. Our preliminary data show that the spectra of the proton and the helium have nearly the same power indices ~2.80, while those of heavier ones become gradually harder as the mass gets heavier, for instance the index is ~2.70 for CNO-group and ~2.55 for Fe-group. It is remarkable that a very high energy proton with multi-PeV is detected in 1995 experiment, and the estimated flux of this event coincides with a simple extrapolation from the energy spectrum with the power index 2.8 observed in the range 10-500 TeV. It indicates that there is no spectral break at around 100 TeV, in contrast to the maximum energy predicted by the current shock-wave acceleration model. This evidence requires some modification on the acceleration and/or propagation mechanism. Also we present all-particle spectrum and the average primary mass in the energy range 20-1000 TeV/particle. Our preliminary data show no drastic change in mass composition over the wide energy range, at least up to 1 PeV/particle, though the statistics is not yet enough to confirm it concretely. The flight performance and the procedure of the analysis, particularly the energy determination methods and the detection efficiency calculation are also given.

AB - We report experimental results obtained by the emulsion chambers on board of the long duration balloon. We have been carrying out the trans-Siberian-continental balloon flight since 1995, and the results from 1995 to 1996 experiments are presented here. Total exposure of these two years amounts to 231.5 m2 h at the average altitude of ~32 km. The energy range covers 10-500 TeV for proton-primary, 3-70 TeV/n for helium-primary, and 1-5 TeV/n for Fe-group (Z=26-28), though statistics of heavy components is not yet enough. Our preliminary data show that the spectra of the proton and the helium have nearly the same power indices ~2.80, while those of heavier ones become gradually harder as the mass gets heavier, for instance the index is ~2.70 for CNO-group and ~2.55 for Fe-group. It is remarkable that a very high energy proton with multi-PeV is detected in 1995 experiment, and the estimated flux of this event coincides with a simple extrapolation from the energy spectrum with the power index 2.8 observed in the range 10-500 TeV. It indicates that there is no spectral break at around 100 TeV, in contrast to the maximum energy predicted by the current shock-wave acceleration model. This evidence requires some modification on the acceleration and/or propagation mechanism. Also we present all-particle spectrum and the average primary mass in the energy range 20-1000 TeV/particle. Our preliminary data show no drastic change in mass composition over the wide energy range, at least up to 1 PeV/particle, though the statistics is not yet enough to confirm it concretely. The flight performance and the procedure of the analysis, particularly the energy determination methods and the detection efficiency calculation are also given.

UR - http://www.scopus.com/inward/record.url?scp=18044399375&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=18044399375&partnerID=8YFLogxK

U2 - 10.1016/S0927-6505(00)00163-8

DO - 10.1016/S0927-6505(00)00163-8

M3 - Article

AN - SCOPUS:18044399375

VL - 16

SP - 13

EP - 46

JO - Astroparticle Physics

JF - Astroparticle Physics

SN - 0927-6505

IS - 1

ER -