## 3 Results
### The Pulsar's Profile Flux vs. ROT Correlation  
Only part of the information collected during the recording of the pulsar signal was used for our analysis. First of all, the frequency range has been narrowed from 118 to 142 MHz (see Figure 3). It was dictated by the need to minimize the impact of disturbances on the relative flux. The observations were conducted in May and August 2017 for J0332+5434, and in April and May 2017 in the case of J1509+5531. The single  
Figure 7: The dynamic spectra for two distant discreet radio sources observed with LBA part of PL612 LOFAR station in Baldy are presented. (**a**) Cyg A observed 2017.05.19; (**b**) Cas A observed 2017.08.19. For both part Y axis denote frequency and X axis shows the time. Color bars representing relative flux received by the system. The structures visible in the figures show changes caused by the ionosphere. session observing time was between a few and a dozen hours, and in this time range we were looking for the pulsar line-of-sight close-ups with GNSS satellites. Our limit connected with the 2\({}^{\circ}\) LOFAR beam size during chosen observation mode was 3 degrees angle in the sky. The Tables 2 and 3 show summary information on the observations. The Figure 6 shows all the close-ups with the limitations presented above. Two columns denote observational status on the sky for three chosen for analysis observation epochs for PSR J0332+5434 and PSR J1509+5531, respectively. The blue lines show the pulsar's path on the celestial sphere as shown in the azimuth coordinate system, in a polar projection. The time of observations is presented in Tables 2 and 3 for both observed pulsars. The dashed lines show the trajectories of the conjunct GNSS satellites. The fragments of the satellite's path in the sky where the distance to the pulsars did not exceed our assumed value of 3 angular degrees are bold and marked in red. For further analysis, the results obtained during the close-ups were collected, i.e., the value of the relative flux averaged for one-minute sub integrations and the ROT values calculated with the same period (see Equation (2)). The main motivation was to search for correlations between changes in the state of the ionosphere towards the pulsar and its relative flux. The correlation coefficients were calculated using Pearson method implemented in Python script. The data we collected is shown in Figure 8. The data has been presented in the similar arrangement of panels as before, so that the Figure 8 is consistent with the Figure 6 when it comes to the layout of the presented content in the panels. The relative flux values for the main component of the pulsar profiles were determined (for all previously designated close-ups) with the minute integration time and then by using Gaussian curve fit. Values obtained are presented in red on the top parts of each panel. For each obtained value of the relative flux, the ROT values were calculated (see Equation (3)) and the results are presented in the lower parts of each panel using the green color. Data from all close-ups in a given pulsar observation epoch (see Tables 2 and 3, columns 1-3) were presented in one sequence. The reason for this is that the correlation applies only to those results that were obtained during the conjunction of the pulsar and the satellite. To be clear, the observation intervals have been marked in vertical tiny dotted lines on each panel, as well as begin and stop of each subsequent was specified on the x axis. Each panel is composed from 2-6 observation intervals corresponding to the satellite-pulsar tracking close-ups (see Figure 5). However, there may occur some random correlation within single observation intervals, the most important correlation information is the inter-dependence of the general trend and interval-to-interval variabilities. This dependence is clearly visible for the J0332+5334 pulsar observed on 20 May 2017 (left middle panel of Figure 7)--one can clearly see a significant increase of the pulsar peak flux during decrease of ROT value.