TY - JOUR
T1 - Precise measurements of cosmic-ray antiproton spectrum in a positive phase of the solar cycle
AU - Maeno, T.
AU - Nozaki, M.
AU - Orito, S.
AU - Matsunaga, H.
AU - Abe, K.
AU - Anraku, K.
AU - Asaoka, Y.
AU - Fujikawa, M.
AU - Imori, M.
AU - Makida, Y.
AU - Matsui, N.
AU - Matsumoto, H.
AU - Mitchell, J.
AU - Mitsui, T.
AU - Moiseev, A.
AU - Motoki, M.
AU - Nishimura, J.
AU - Ormes, J.
AU - Saeki, T.
AU - Sanuki, T.
AU - Sasaki, M.
AU - Seo, E. S.
AU - Shikaze, Y.
AU - Sonoda, T.
AU - Streitmatter, R.
AU - Suzuki, J.
AU - Tanaka, K.
AU - Ueda, I.
AU - Wang, J. Z.
AU - Yajima, N.
AU - Yamagami, T.
AU - Yamamoto, A.
AU - Yoshida, T.
AU - Yoshimura, K.
N1 - Funding Information:
using the computing facilities at ICEPP, Univ. of Tokyo. This experiment was supported by Grant-in-Aid for Scientific Research in Monbusho, Heiwa Nakajima Foundation in Japan, and by NASA in the USA.
PY - 2001
Y1 - 2001
N2 - The BESS spectrometer has measured the energy spectrum of cosmic-ray antiprotons successively in 1993, 1995, 1997 and 1998. In total, 848 antiprotons were clearly identified in energy range 0.18 to 4.20 GeV based on magnetic-rigidity, time-of-flight, energy loss, and Cherenkov radiation measurements. The measured antiproton spectra and antiproton/proton ratios were nearly identical at the upper end of the instrumental energy range, which is consistent with theoretical calculations. In the low energy region, our data show variations that are somewhat larger than expected. This might be due to statistical fluctuation, or might suggest a contribution of primary antiprotons from novel sources.
AB - The BESS spectrometer has measured the energy spectrum of cosmic-ray antiprotons successively in 1993, 1995, 1997 and 1998. In total, 848 antiprotons were clearly identified in energy range 0.18 to 4.20 GeV based on magnetic-rigidity, time-of-flight, energy loss, and Cherenkov radiation measurements. The measured antiproton spectra and antiproton/proton ratios were nearly identical at the upper end of the instrumental energy range, which is consistent with theoretical calculations. In the low energy region, our data show variations that are somewhat larger than expected. This might be due to statistical fluctuation, or might suggest a contribution of primary antiprotons from novel sources.
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U2 - 10.1016/S0273-1177(01)00129-6
DO - 10.1016/S0273-1177(01)00129-6
M3 - Article
AN - SCOPUS:6644229655
SN - 0273-1177
VL - 27
SP - 711
EP - 716
JO - Advances in Space Research
JF - Advances in Space Research
IS - 4
ER -