The cosmic-ray energy spectrum between 1014.5 and 1016.3 eV covering the "knee" region

M. Amenomori*, Z. Cao, B. Z. Dai, L. K. Ding, Y. X. Feng, Z. Y. Feng, K. Hibino, N. Hotta, Q. Huang, A. X. Huo, H. Y. Jia, G. Z. Jiang, S. Q. Jiao, F. Kajino, K. Kasahara, Labaciren, S. M. Liu, D. M. Mei, L. Meng, X. R. MengMimaciren, K. Mizutanin, J. Mu, H. Nanjo, M. Nlshizawa, M. Ohnishi, I. Ohta, T. Ouchi, J. R. Ren, T. U. Saito, M. Sakata, Z. Z. Shi, M. Shibata, A. Shiomi, T. Shirai, H. Sugimoto, X. X. Sun, K. Taira, Y. H. Tan, N. Tateyama, Shoji Torii, H. Wang, C. Z. Wen, Y. Yamamoto, G. C. Yu, P. Yuan, T. Yuda, C. S. Zhang, H. M. Zhang, L. Zhang, Zhasang, Zhaxiciren, W. D. Zhou

*この研究の対応する著者

研究成果: Article査読

79 被引用数 (Scopus)

抄録

The Tibet array is the first air shower detector to search for 10 TeV gamma-ray point sources. This array also has a high sensitivity to air showers initiated by cosmic rays around the "knee" of the all-particle spectrum at 1015-1016 eV, with quite small ambiguity for the energy estimation, since the development of air showers in this high energy region is close to maximum at Yangbajing altitude (4300 m above sea level). Using the data set taken with the Tibet array in the period from 1990 October through 1993 July, we obtained the differential energy spectrum of primary cosmic rays between 3 × 1014 and 2 × 1016 eV covering the knee region. The overall spectrum obtained does not resemble a single power law and shows a gradual steepening of the slope at energies around 1015.25 eV. The spectrum is expressed as J(E0) = 1.5 × 10-20(E0/1014.75 eV)-2.60±0.04(m-2 s-1 sr-1 eV-1) at E0 < 1014.75 eV and J(E0) = 1.2 × 10-23(E0/1015.85 eV)-3.00±0.05(m-2 s-1 sr-1 eV-1) at E0 > 1015.85 eV, where this changes gradually between 1014.75 and 1015.85 eV and takes the value J(E0) = 6.7 × 10-22 (m-2 s-1 sr-1 eV-1) at E0 = 1015.25 eV.

本文言語English
ページ(範囲)408-414
ページ数7
ジャーナルAstrophysical Journal
461
1 PART I
出版ステータスPublished - 1996
外部発表はい

ASJC Scopus subject areas

  • 宇宙惑星科学

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