The iron emission lines Kα and Kβ in active galactic nuclei — A further piece of evidence for the Cerenkov line-like radiation |
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| Institution: | 1. Institute of Space and Astrophysics, Department of Physics, Shanghai Jiao Tong University, Shanghai 200030, China;2. Institute of Astronomy, Department of Physics, Taiwan Central University, Taipei 32054, Taiwan;1. Department of Frontier Materials, Graduate School of Engineering, Nagoya Institute of Technology, Showa-ku, Nagoya 466-8555, Japan;2. Department of Materials Science and Engineering, Graduate School of Engineering, Nagoya Institute of Technology, Showa-ku, Nagoya 466-8555, Japan;1. State Key Laboratory of Rare Earth Resource Utilization, Changchun Institute of Applied Chemistry, Chinese Academy of Sciences, Changchun 130022, China;2. State Key Laboratory of Fine Chemicals, PSU-DUT Joint Center for Energy Research, School of Chemical Engineering, Dalian University of Technology, Dalian 116024, China;1. Computational Imaging, Centrum Wiskunde & Informatica, Science park 123, 1098XG Amsterdam, Netherlands;2. Institute of Multidisciplinary Research for Advanced Materials, Tohoku University, Katahira 2-1-1, Aoba-ku, Sendai 980-8577, Japan;3. Ernst Ruska-Centre for Microscopy and Spectroscopy with Electrons and Peter Grünberg Institute, Forschungszentrum Jülich, D-52425 Jülich, Germany;4. EMAT, University of Antwerp, Groenenborgerlaan 171, B-2020 Antwerp, Belgium;5. Laboratory of Adsorption and Catalysis, Department of Chemistry, University of Antwerp, Universiteitsplein 1, 2610 Wilrijk, Belgium;6. European Technology Center, ExxonMobil Chemical Europe Inc., Hermeslaan 2, B-1831 Machelen, Belgium |
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| Abstract: | It has been recently observed by XMM-Newton that besides the emission line of iron Kα at 6.4 keV there also exists in the Seyfert 1 galaxy NGC 3783 the very intense emission line of iron Kβ at 7.0 keV. Moreover, the ratio of equivalent widths (EWs) of these two lines can hardly be interpreted with the traditional mechanism of “photoelectric absorption — fluorescence emission”. By using the mechanism of Cerenkov line-like radiation proposed by YOU Jun-hian et al., the ratio of EWKα/EWKβ may be reasonably interpreted by means of a detailed model theoretical computation. As shown by the results, the iron K lines in active galactic nuclei (AGNs) are formed not only by the fluorescence mechanism, but also by the Cerenkov line-like radiation. Both coexist in AGNs, with the latter playing the dominant role. |
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