宇宙MeVガンマ線背景放射と活動銀河核の硬X線スペクトル：AGNのホットコロナの起源への示唆
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(112) DDE12)ef'g. 11) Galeev A. A., Rosner R., Vaiana G. S., 1979, ApJ 229, 318 12) Liu B. F., Mineshige S., Shibata K., 2002, ApJ 572, L173 13) Pozdniakov L. A., Sobol I. M., Siuniaev R. A., 1977, AZh 54, 1246 14) Gorecki A., Wilczewski W., 1984, Acta Astron. 34, 141 15) Gruber D. E., Matteson J. L., Peterson L. E., Jung G. V., 1999, ApJ 520, 124 16) Kappadath S. C., et al., 1996, A&AS 120, 619 17) Inoue Y., Totani T., Ueda Y., 2008, ApJ 672, L5 18) Lin R. P., 2006, Space Sci. Rev. 124, 233 19) Øieroset M., Lin R. P., Phan T. D., Larson D. E., Bale S. D., 2002, Phys. Rev. Lett. 89, 195001 20) Boggs S. E., 2006, NewA Rev. 50, 604. + $% h$i jk MeV lmn opqr
(113) as. D AGN tY. tYuW'23478vwVW'xyz H %. ῐ. ῏. {|9}~i r 17)h($H '% }~ o#rh'%. ῎῍ῑῌ 1) Ueda Y., Akiyama M., Ohta K., Miyaji T., 2003, ApJ 598, 886 2) Gilli R., Comastri A., Hasinger G., 2007, A&A 463, 79 3) Sreekumar P., et al., 1998, ApJ 494, 523 4) Narumoto T., Totani T., 2006, ApJ 643, 81 5) Watanabe K., Hartmann D. H., Leising M. D., The L.-S., 1999, ApJ 516, 285 6) Strigari L. E., Beacom J. F., Walker T. P., Zhang P., 2005, J. Cosmol. Astropart. Phys. 4, 17 7) Ahn K., Komatsu E., 2005, Phys. Rev. D 71, 021303 8) Totani T., 2006, PASJ 58, 965 9) Zdziarski A. A., Fabian A. C., Nandra K., Celotti A., Rees M. J., Done C., Coppi P. S., Madejski G. M., 1994, MNRAS 269, L55 10) Zdziarski A. A., Poutanen J., Johnson W. N., 2000, ApJ 542, 703. 396. The Cosmic MeV Gamma-ray Background and Hard X-ray Spectra of Active Galactic Nuclei: Implications for the Origin of Hot AGN Coronae Yoshiyuki INOUE Department of Astronomy, Kyoto University, Oiwake-cho, Kitashirakawa, Sakyo-ku, Kyoto 606ῌ 8502, Japan Abstract : The origin of the extragalactic MeV gamma-ray background radiation is still unknown. Current AGN spectrum models which explain the cosmic X-ray background cannot explain the MeV background spectrum, because of the thermal exponential cuto#. Here we construct a new spectral model including nonthermal coronal electrons, which are expected to exist in a magnetic reconnection heating corona. We show that the MeV background spectrum can nicely be explained by our model and discussed the properties of such nonthermal electrons comparing with those in solar flares and the Earth magnetosphere.. . 2008 7 .
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