Precision Measurement of Cosmic-Ray Antiproton Spectrum
S. Orito(The University of Tokyo), T. Maeno(The University of Tokyo), H. Matsunaga(The University of Tokyo), K. Abe(The University of Tokyo), K. Anraku(The University of Tokyo), Y. Asaoka(The University of Tokyo), M. Fujikawa(The University of Tokyo), M. Imori(The University of Tokyo), M. Ishino(Kyoto University), Y. Makida(High Energy Accelerator Research Organization), N. Matsui(The University of Tokyo), H. Matsumoto(Kobe University), J. Mitchell(Goddard Space Flight Center), T. Mitsui(Kobe University), A. A. Moiseev(National Aeronautics and Space Administration), M. Motoki(The University of Tokyo), Jun Nishimura(The University of Tokyo), M. Nozaki(Kobe University), J. F. Ormes(National Aeronautics and Space Administration), T. Saeki(The University of Tokyo), T. Sanuki(The University of Tokyo), M. Sasaki(Kobe University), E. S. Seo(University of Maryland, College Park), Y. Shikaze(The University of Tokyo), T. Sonoda(The University of Tokyo), R. E. Streitmatter(Goddard Space Flight Center), Jun Suzuki(High Energy Accelerator Research Organization), К. Таnака(High Energy Accelerator Research Organization), I. Ueda(The University of Tokyo), Nobuyuki Yajima(Institute of Space and Astronautical Science), T. Yamagami(Institute of Space and Astronautical Science), Akira Yamamoto(High Energy Accelerator Research Organization), T. Yoshida(High Energy Accelerator Research Organization), K. Yoshimura(The University of Tokyo)
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Abstract
The energy spectrum of cosmic-ray antiprotons ( &pmacr;'s) has been measured in the range 0.18-3.56 GeV, based on 458 &pmacr;'s collected by BESS in a recent solar-minimum period. We have detected for the first time a characteristic peak at 2 GeV of &pmacr;'s originating from cosmic-ray interactions with the interstellar gas. The peak spectrum is reproduced by theoretical calculations, implying that the propagation models are basically correct and that different cosmic-ray species undergo a universal propagation. Future BESS data with still higher statistics will allow us to study the solar modulation and the propagation in detail and to search for primary &pmacr; components.
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