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Title:
The acceleration of cosmic-ray protons in the supernova remnant RX J1713.7-3946
Authors:
Enomoto, R.; Tanimori, T.; Naito, T.; Yoshida, T.; Yanagita, S.; Mori, M.; Edwards, P. G.; Asahara, A.; Bicknell, G. V.; Gunji, S.; Hara, S.; Hara, T.; Hayashi, S.; Itoh, C.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kataoka, J.; Kawachi, A.; Kifune, T.; Kubo, H.; Kushida, J.; Maeda, S.; Maeshiro, A.; Matsubara, Y.; Mizumoto, Y.; Moriya, M.; Muraishi, H.; Muraki, Y.; Nakase, T.; Nishijima, K.; Ohishi, M.; Okumura, K.; Patterson, J. R.; Sakurazawa, K.; Suzuki, R.; Swaby, D. L.; Takano, K.; Takano, T.; Tokanai, F.; Tsuchiya, K.; Tsunoo, H.; Uruma, K.; Watanabe, A.; Yoshikoshi, T.
Affiliation:
AA(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan), AB(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan), AC(Faculty of Management Information, Yamanashi Gakuin University, Kofu, Yamanashi 400-8575, Japan), AD(Faculty of Science, Ibaraki Unibersity, Mito, Ibaraki 310-8512, Japan), AE(Faculty of Science, Ibaraki Unibersity, Mito, Ibaraki 310-8512, Japan), AF(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan), AG(Institute of Space and Astronautical Science, Sagamihara, Kanagawa 229-8510, Japan), AH(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan), AI(Mt Stromlo and Siding Spring Observatories, Australian National University, ACT 2611, Australia), AJ(Department of Physics, Yamagata University, Yamagata, Yamagata 900-8560, Japan), AK(Department of Physics, Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8551, Japan), AL(Faculty of Management Information, Yamanashi Gakuin University, Kofu, Yamanashi 400-8575, Japan), AM(Department of Physics, Konan University, Kobe, Hyogo 658-8501, Japan), AN(Faculty of Science, Ibaraki Unibersity, Mito, Ibaraki 310-8512, Japan), AO(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan), AP(Department of Physics, Konan University, Kobe, Hyogo 658-8501, Japan), AQ(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan), AR(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan), AS(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan), AT(Faculty of Engineering, Shinshu University, Nagano, Nagano 380-8553, Japan), AU(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan), AV(Department of Physics, Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8551, Japan), AW(Department of Physics, Konan University, Kobe, Hyogo 658-8501, Japan), AX(Department of Physics, Konan University, Kobe, Hyogo 658-8501, Japan), AY(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi 464-8601, Japan), AZ(National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan), BA(Department of Physics, Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8551, Japan), BB(Ibaraki Prefectural University of Health Sciences, Ami, Ibaraki 300-0394, Japan), BC(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi 464-8601, Japan), BD(Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan), BE(Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan), BF(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan), BG(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan), BH(Department of Physics and Mathematical Physics, University of Adelaide, SA 5005, Australia), BI(Department of Physics, Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8551, Japan), BJ(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan), BK(Department of Physics and Mathematical Physics, University of Adelaide, SA 5005, Australia), BL(Department of Physics, Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8551, Japan), BM(Department of Physics, Yamagata University, Yamagata, Yamagata 900-8560, Japan), BN(Department of Physics, Yamagata University, Yamagata, Yamagata 900-8560, Japan), BO(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan), BP(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan), BQ(Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan), BR(Department of Physics, Yamagata University, Yamagata, Yamagata 900-8560, Japan), BS(Department of Physics, Osaka City University, Osaka, Osaka 558-8585, Japan)
Publication:
Nature, Volume 416, Issue 6883, pp. 823-826 (2002). (Nature Homepage)
Publication Date:
04/2002
Origin:
NATURE
DOI:
10.1038/416823a
Bibliographic Code:
2002Natur.416..823E

Abstract

Protons with energies up to ~1015eV are the main component of cosmic rays, but evidence for the specific locations where they could have been accelerated to these energies has been lacking. Electrons are known to be accelerated to cosmic-ray energies in supernova remnants, and the shock waves associated with such remnants, when they hit the surrounding interstellar medium, could also provide the energy to accelerate protons. The signature of such a process would be the decay of pions (π0), which are generated when the protons collide with atoms and molecules in an interstellar cloud: pion decay results in γ-rays with a particular spectral-energy distribution. Here we report the observation of cascade showers of optical photons resulting from γ-rays at energies of ~1012eV hitting Earth's upper atmosphere, in the direction of the supernova remnant RX J1713.7-3946. The spectrum is a good match to that predicted by pion decay, and cannot be explained by other mechanisms.
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