## 3 Results
### The Pulsar's Profile Flux vs. ROT Correlation
For a better insight to the general trend, each plot is \begin{table}
\begin{tabular}{c c c c c c c c c} \hline \hline \multirow{2}{*}{**Date**} & **Start** & **End** & **S/N 2** & **Relative** & **ROT 2** & **No of** & **No of** & **Correlation** \\  & **Time 1** & **Time 1** & **Time 1** & **Flux 2** & **ROT 2** & **Close-Ups** & **Points** & **Coefficient 3** \\ \hline
19 May 2017 & 15:00 & 23:59 & 131.6 & 2.08 & 0.294 & 3 & 13 & \(-\)0.743 \\
20 May 2017 & 00:00 & 20:00 & 184.4 & 3.41 & 0.334 & 6 & 50 & \(-\)0.571 4 \\
19 August & 00:00 & 8:00 & 396.9 & 7.75 & 0.042 & 2 & 13 & \(-\)0.138 \\
2017 & \multicolumn{1}{c}{\({}^{1}\) UT, 2 Max value, 3 For all measured points; 4 Mean value.} & & & & & \\ \hline \hline \end{tabular}
\end{table} 
Table 2: The summary of measuring data for PSR J0332+5434. \begin{table}
\begin{tabular}{c c c c c c c c c} \hline \hline \multirow{2}{*}{**Date**} & **Start** & **End** & **S/N 2** & **Relative** & **ROT 2** & **No of** & **No of** & **Correlation** \\  & **Time 1** & **Time 1** & **Time 1** & **Flux 2** & **ROT 2** & **Close-Ups** & **Points** & **Coefficient 3** \\ \hline
10 April 2017 & 00:00 & 04:30 & 218.5 & 2.44 & 0,114 & 4 & 27 & \(-\)0.468 \\
8 May 2017 & 00:00 & 05:30 & 96.1 & 0.94 & 0,082 & 4 & 27 & \(-\)0.712 \\
13 May 2017 & 00:00 & 15:30 & 93.4 & 0.91 & 0,270 & 4 & 27 & \(-\)0.468 \\ \hline \hline \end{tabular} \({}^{1}\) UT, 2 Max value; 3 For all measured points.  
\end{table} 
Table 3: The summary of measuring data for PSR J1509+5531. complemented with a linear trend, however the trend line for J0332+5334 pulsar observed on 20 May 2017 (left middle panel of Figure 7) was split into two trends: before ROT jump and after. In this single case the total observation time span was significantly longer and the discontinuity both in ROT and pulsar peak flux was more than evident. The weakest correlation may be noted on the lower left panel of Figure 7 (J0332+5334 pulsar observed on 19 August 2017), the correlation coefficient around \(-0.14\). Such situation is caused by two factors--number of observing points was low (only 13), ROT value was in general very small (maximum below 0.05), the result of which lead to mostly random correlations. That also explains correlation calculation between whole datasets--variability within the short intervals may lead to random, unreliable results. Taking into account situations of higher ROT values and variability, the general trend is obvious--stronger fluctuations of TEC are'seen' in the pulsar profiles as a decrease of the radio flux peak value. The significance of the existence of such an anti-correlation on the typical measured level from \(-0.46\) to \(-0.74\) is considerable (only one value in Table 2 is below of this range). It clearly shows that for certain specific types of observations (long waves and relatively short duration), changes in the measured parameters are closely related to the density of ions in the ionosphere layer. Without taking into account the influence of the ionosphere, our interpretation, which refers to astrophysical phenomena, may lead to false conclusions. In order to check whether the signals from satellites above the horizon in other areas of the sky show significant similarities, we selected satellites visible during our measurements and combined the ROT data with the ROT data from satellites observed towards the pulsar-one observation epoch for each. Data is presented in Figure 9. The left plot is the visibility of GNSS satellites during observations of PSR J0332+5434 with regions, where data was taken from marked in bold. The close-up to the R16 satellite (20 May 2017 from 0:56 to 1:06 UT) is marked in red. The same time for the rest of satellites is marked in blue at their paths. This plot is made in the azimuth coordinate system in a polar projection, what is similar to way of presentation in Figure 6. It is worth paying attention to the right part of Figure 9, where the ROT values towards a set of satellites are presented.