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Fig. 8.


νf(ν) flux at 0.5, 4.5 keV and the power-law energy spectral index of the blazar OJ 287 are plotted against observation date. Many differences in the top and middle panels are clearly visible; in particular, the X-ray flares occur in different periods in the soft (0.5 keV) and hard (4.5 keV) parts of the X-ray spectrum.

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