X-ray Emissions of Fermi Blazarstwo |
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Authors: | Yang Jiang-he Fan Jun-hui Zhang Yue-lian Yang Ru-shu Tuo Man-xian Nie Jian-jun |
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Institution: | 1. Department of Physics and Electronics Science, Hunan University of Arts and Science, Changde 415000;2. Center for Astrophysics, Guangzhou University, Guangzhou 510006;3. Astronomy Science and Technology Research Laboratory of Department of Education of Guangdong Province, Guangzhou 510006;4. Mathematics and Computational Science, Hunan University of Arts and Science, Changde 415000 |
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Abstract: | The X-ray emissions of blazars are located at the end of synchrotron radiation and the beginning of inverse Compton radiation. Therefore, the origin of the X-ray emissions is rather complex. The spectral energy distributions (SEDs) of blazars from radio to X-ray bands can be fitted approximatively by a parabolic function. If we consider approximately the fitting curves as the physical spectra of blazars to analyze the X-ray emissions of Fermi blazars, the results show that: (1) The X-ray emissions of blazars contain two components, i.e. the synchrotron radiation and inverse Compton radiation, which can be simply separated by these fitting curves; (2) the higher the synchrotron peak frequency of the source, the greater the synchrotron radiation component, and the less the inverse Compton radiation component; (3) at 1 keV of the X-ray waveband, the synchrotron radiation component accounts for 17%, 27%, and 73% of the total X-ray emission, for FSRQs (Flat Spectrum Radio Quasars), LBLs (Low synchrotron peak frequency BL Lac objects), and HBLs (High synchrotron peak frequency BL Lac objects), respectively; (4) there is a strong positive correlation between the synchrotron peak frequency and the synchrotron radiation flux density at 1 keV, while no correlation exists between the synchrotron peak frequency and the inverse Compton radiation flux density; (5) the radiation mechanism of LBLs may be similar to that of FSRQs in the X-ray waveband. |
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Keywords: | Galaxies: active Radiation mechanisms: non-thermal X-rays: galaxies methods: statistical |
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