@inproceedings{oai:jaxa.repo.nii.ac.jp:00004936,
 author = {井岡, 邦仁 and 川中, 宣太 and 野尻, 美保子 and 藤田, 裕 and 郡, 和範 and 山崎, 了 and Ioka, Kunihito and Kawanaka, Norita and Nojiri, Mihoko M. and Fujita, Yutaka and Kohri, Kazunori and Yamazaki, Ryo and Meszaros, Peter},
 book = {宇宙航空研究開発機構特別資料:, JAXA Special Publication: The Energetic Cosmos; from Suzaku to ASTRO-H},
 month = {Feb},
 note = {The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, We discuss that a nearby astrophysical source, such as pulsar, supernova remnant or gamma-ray burst (GRB), about 10(exp 5-6) years ago may be responsible for the excesses of cosmic-ray positrons and electrons recently observed by the PAMELA, ATIC/PPB-BETS, Fermi and HESS experiments. We can reproduce the smooth Fermi/HESS spectra as well as the spiky ATIC/PPB-BETS spectra. The spectra can possess a sharp cutoff that is similar to the dark matter predictions since higher energy cosmic-rays cool faster where the cutoff energy marks the source age. A burst-like astrophysical source is expected to have a small but finite spread in the cutoff as well as anisotropy in the cosmic-ray and diffuse gamma-ray flux, providing a method for the Fermi and future CALET experiments to discriminate between dark matter and astrophysical origins and also to constrain the source duration. Whether the source is leptonic or hadronic may be probed by the antiprotons. Such GRB-like sources may leave remnants observed as mysterious TeV unidentified sources., Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science, 資料番号: AA0064574004, レポート番号: JAXA-SP-09-008E},
 pages = {14--17},
 publisher = {宇宙航空研究開発機構, Japan Aerospace Exploration Agency (JAXA)},
 title = {Cosmic-Ray Positrons from Astrophysical Sources: GRBs, Pulsars and SNRs},
 volume = {JAXA-SP-09-008E},
 year = {2010}
}