Figure 1: Flux density variations over 400 min at four frequencies. | |
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Figure 2: Cross-correlation coefficients of the flux variations in dependence on frequency separation corrected for noise. | |
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Figure 3: Structure function of intensity variations normalized by the mean intensity in the time domain at a frequency of 4640 MHz corrected for noise. | |
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Figure 4: Mean auto- (top) and cross-correlation (bottom) function between successive spectra in dependence on frequency lag. One frequency lag corresponds to 19.5 kHz. The data points are averaged over 70 min. | |
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Figure 5: Mean auto- (top) and cross-correlation (bottom) function at f = 610 MHz in dependence on time lag. One time lag corresponds to 59 s. The data points are averaged over 1024 frequency channels. | |
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Figure 6: Mean time structure function of intensity variations at f = 610 MHz corrected for noise as described in the text and normalized by 2 m^{2}, where m is the modulation index. The line is a fit to the first points. | |
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Figure 7: Mean frequency structure function of intensity variations at f = 610 MHz corrected for noise as described in the text and normalized by 2 m^{2}, where m is the modulation index. The line is a fit to the first points. | |
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Figure 8: Time structure function of phase fluctuations at f_{0} = 1 GHz as compiled from the following data points 1.) 102 MHz observations: filled circles; 2.) 610 MHz: open circles; 3.) 5 GHz: stars. The solid line corresponds to the best fit to the first points of the structure functions. The slope is 1.50. The dashed line corresponds to n = 1.67 (Kolmogorov model). | |
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Figure 9: Frequency structure function of phase fluctuations at f_{0} = 1 GHz based on data at 102 MHz, 610 MHz and 5 GHz (the different frequencies are characterized by different sizes of the circles) for two models: 1.) diffractive scintillation model; 2.) model with angular refraction. The solid line corresponds to the best fit to the first data points of the structure function. The slope is 1.47. | |
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Figure 10: Structure function of phase fluctuations at f_{0} = 1 GHzversus spatial scale of the inhomogeneities. The signs are the same as in Fig. 8; the cross designates the value computed from an analysis of refractive scintillation; the point at 10^{14} m is an upper limit from timing observations at 102 MHz. The points at the highest spatial scales are from DM variations of pulsar pairs in globular clusters. The line 1 corresponds to the best fit to the first points of the structure function, the line 2 to the Kolmogorov spectrum, and the line 3 is computed from Eqs. (41) and (44) as explained in the text. | |
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