Azimuthally controlled observation of heavy cosmic-ray primaries by means of the balloon-borne emulsion chamber

E. Kamioka, M. Hareyama, M. Ichimura, Y. Ishihara, T. Kobayashi, H. Komatsu, S. Kuramata, K. Maruguchi, H. Matsutani, A. Mihashi, H. Mito, T. Nakamura, H. Nanjo, T. Ouchi, T. Ozawa, T. Shibata, H. Sugimoto, Z. Watanabe

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Abstract

We have exposed an emulsion chamber with an area of 1.22 m2 on board of the balloon at an atmospheric depth of 8.9 g/cm2 for 15.8 h, which has been azimuthally controlled within the accuracy of Δφ = 0.5°. With the use of the east-west asymmetry effect of arriving cosmic-ray primaries, we can obtain the energy spectra for individual elements in the kinetic energy range from a few GeV/nucleon up to ∼ 15 GeV/nucleon. We present also the energy spectra obtained by the opening-angle method for the higher energy region, 5-1000 GeV/nucleon, for the elements not lighter than silicon. We find that the energy spectra obtained by the former method continue smoothly to those obtained by the latter, indicating that the energy determination using the opening-angle method is performed correctly. We compare also the present results with those obtained by the previous work. We find that the iron flux is in nice agreement with that obtained by the previous observation, the differential spectral index being constant, ∼ 2.5, up to a few TeV/nucleon, while in the case of the silicon component, it is ∼ 2.7 for 10-1000 GeV/nucleon in this work, significantly harder than the previous one, ∼ 2.9. We also report the flux of the sub-iron component and its abundance ratio to the iron component. We find the abundance ratio of [Z = 21-25]/iron is slightly less than those obtained previously in the higher energy region, ≥ 100 GeV/n.

Original languageEnglish
Pages (from-to)155-167
Number of pages13
JournalAstroparticle Physics
Volume6
Issue number2
Publication statusPublished - 1997 Feb
Externally publishedYes

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heavy cosmic ray primaries
balloons
emulsions
chambers
iron
energy spectra
primary cosmic rays
silicon
energy
kinetic energy
asymmetry

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

Cite this

Kamioka, E., Hareyama, M., Ichimura, M., Ishihara, Y., Kobayashi, T., Komatsu, H., ... Watanabe, Z. (1997). Azimuthally controlled observation of heavy cosmic-ray primaries by means of the balloon-borne emulsion chamber. Astroparticle Physics, 6(2), 155-167.

Azimuthally controlled observation of heavy cosmic-ray primaries by means of the balloon-borne emulsion chamber. / Kamioka, E.; Hareyama, M.; Ichimura, M.; Ishihara, Y.; Kobayashi, T.; Komatsu, H.; Kuramata, S.; Maruguchi, K.; Matsutani, H.; Mihashi, A.; Mito, H.; Nakamura, T.; Nanjo, H.; Ouchi, T.; Ozawa, T.; Shibata, T.; Sugimoto, H.; Watanabe, Z.

In: Astroparticle Physics, Vol. 6, No. 2, 02.1997, p. 155-167.

Research output: Contribution to journalArticle

Kamioka, E, Hareyama, M, Ichimura, M, Ishihara, Y, Kobayashi, T, Komatsu, H, Kuramata, S, Maruguchi, K, Matsutani, H, Mihashi, A, Mito, H, Nakamura, T, Nanjo, H, Ouchi, T, Ozawa, T, Shibata, T, Sugimoto, H & Watanabe, Z 1997, 'Azimuthally controlled observation of heavy cosmic-ray primaries by means of the balloon-borne emulsion chamber', Astroparticle Physics, vol. 6, no. 2, pp. 155-167.
Kamioka E, Hareyama M, Ichimura M, Ishihara Y, Kobayashi T, Komatsu H et al. Azimuthally controlled observation of heavy cosmic-ray primaries by means of the balloon-borne emulsion chamber. Astroparticle Physics. 1997 Feb;6(2):155-167.
Kamioka, E. ; Hareyama, M. ; Ichimura, M. ; Ishihara, Y. ; Kobayashi, T. ; Komatsu, H. ; Kuramata, S. ; Maruguchi, K. ; Matsutani, H. ; Mihashi, A. ; Mito, H. ; Nakamura, T. ; Nanjo, H. ; Ouchi, T. ; Ozawa, T. ; Shibata, T. ; Sugimoto, H. ; Watanabe, Z. / Azimuthally controlled observation of heavy cosmic-ray primaries by means of the balloon-borne emulsion chamber. In: Astroparticle Physics. 1997 ; Vol. 6, No. 2. pp. 155-167.
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AU - Kamioka, E.

AU - Hareyama, M.

AU - Ichimura, M.

AU - Ishihara, Y.

AU - Kobayashi, T.

AU - Komatsu, H.

AU - Kuramata, S.

AU - Maruguchi, K.

AU - Matsutani, H.

AU - Mihashi, A.

AU - Mito, H.

AU - Nakamura, T.

AU - Nanjo, H.

AU - Ouchi, T.

AU - Ozawa, T.

AU - Shibata, T.

AU - Sugimoto, H.

AU - Watanabe, Z.

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AB - We have exposed an emulsion chamber with an area of 1.22 m2 on board of the balloon at an atmospheric depth of 8.9 g/cm2 for 15.8 h, which has been azimuthally controlled within the accuracy of Δφ = 0.5°. With the use of the east-west asymmetry effect of arriving cosmic-ray primaries, we can obtain the energy spectra for individual elements in the kinetic energy range from a few GeV/nucleon up to ∼ 15 GeV/nucleon. We present also the energy spectra obtained by the opening-angle method for the higher energy region, 5-1000 GeV/nucleon, for the elements not lighter than silicon. We find that the energy spectra obtained by the former method continue smoothly to those obtained by the latter, indicating that the energy determination using the opening-angle method is performed correctly. We compare also the present results with those obtained by the previous work. We find that the iron flux is in nice agreement with that obtained by the previous observation, the differential spectral index being constant, ∼ 2.5, up to a few TeV/nucleon, while in the case of the silicon component, it is ∼ 2.7 for 10-1000 GeV/nucleon in this work, significantly harder than the previous one, ∼ 2.9. We also report the flux of the sub-iron component and its abundance ratio to the iron component. We find the abundance ratio of [Z = 21-25]/iron is slightly less than those obtained previously in the higher energy region, ≥ 100 GeV/n.

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