## 3 Results
### The Pulsar's Profile Flux vs. ROT Correlation
We took a slightly wider range of time, and the moment of close-up of the R16 satellite with the pulsar is marked with horizontal dotted lines. This plot clearly shows that the ROT parameter measured in different directions in the sky shows significant differences. The above considerations and measurements may lead to a clear conclusion that LOFAR is extremely sensitive to even slight changes in the state of the ionosphere towards observation. The large influence of the ionosphere on the level of the signal reaching the Earth from distant galactic and extragalactic objects such as rotating neutron stars, observed as pulsars is easy to see not only by the anti-correlation between ROT and relative flux shown in the Figure 8.  
Figure 10 represents the general trend slope parameter estimated within the ROT and pulsar peak intensity series. Comparison of the slope parameters of the corresponding time-series reveals the ROT and pulsar intensity series anti-correlation in the terms of the general trend. It can be clearly seen that slope parameters for each pair of corresponding series have opposite values--positive slope for ROT series corresponds with a negative slope of the pulsar intensity series and vice versa. Figure 11 presents the PSR J0332+5434 peak intensity during the 20-h long observation period (00-20 UT) as well as general behavior of ROTI over the different geographic latitudes. One can clearly see that the pulsar peak intensity is lower during the nighttime and rises after the sunset. On the pulsar plot we have also marked the LOFAR-GNSS close-ups to exaggerate that close-ups cover different phases of the pulsar's intensity diurnal variation. The height of the pulsar above the horizon and the signal-to-noise ratio (S/N) are also shown in Figure 11. This data has been included to make it clear that flux fluctuations, which are the largest during the day, are not associated with an increased amount of noise associated with the LOFAR sensor characteristic ([PERSON], 2017). ROTI colormap in Figure 11 is based on observations collected from the chain of GNSS stations along the  
meridian of 20\({}^{\circ}\) E longitude in order to assess the ROTI diurnal behavior. The auroral ionospheric irregularities oval spreads towards lower latitudes during night [56; 57; 58]. That ROTI behavior and night-side auroral oval expanse towards lower latitudes corresponds with the diminishing pulsar intensity observed with LOFAR during night. However significant ROTI values reach 60\({}^{\circ}\) N, it should be remembered, that ROTI is a quantified index of the nominal ROT behavior (here, a hourly average is presented), and thus smaller fluctuations, such as presented ones, might be smoothed out by the long averaging intervals. ROTI variation should be treated as a background--more detailed comparison of the nominal ROT and peak density are presented above and confirm the anti-correlation. Figure 8: Comprehensive presentation of comparison of results of pulsar profile’s relative flux (upper panels, red lines) and Rate of TEC (ROT) (lower panels, green lines) values taken from GNSS data (see Section 3.1). In each panel, all observation points corresponding to all recorded close-ups of the satellite and pulsar in the sky were collected. Vertical lines separate individual close-ups. Each plot is complemented with a linear trend dotted line. Figure 10: Linear trend slope parameters of the ROT and pulsar peak intensity series. Figure 9: The Example of ROT data for one close-up PSR J0332+5434 and R16 satellite (red bold line) compiling the ROT in the direction of the other satellites observed at the same time (blue lines). The (**a**) is the visibility of GNSS satellites (dashed lines) during observations of PSR J0332+5434 (solid line) presented in the azimuth coordinate system in a polar projection. The (**b**) is the relative ROT value taken from the observation on 20 May 2017, from 0:44 to 1.21 UT. The moment of close-up is indicated by dotted horizontal lines.