## 3 Results
### Ionospheric Behavior and GNSS Positioning Errors by Region  
To study the effects of the eclipse, we selected 24 stations from among the 2337 GNSS stations (see Figure 1). We chose five GNSS stations close to the annular solar eclipse (KMOR, KAGZ, MARG, IQAL, PICL). There were six GNSS stations located in the partial eclipse region (CN00, TRO1, SVTL, TIXI, MAG0, YAKT). Furthermore, we used five stations located in the Caribbean and South America (LMMF, BOAV, PIFL, MSBL). The sunrise (in PICL and CN00 stations) and the sunset (in MAG0 and YAKT stations) happened during the eclipse time window at ground level but did not take place at the ionospheric height of 350 km. More details about the GNSS stations and eclipse conditions (with respect to the ionospheric height of 350 km) can be found in Table 1.  
Figure 7: Behavior of the maximum 3D positioning error, 3D-RMS, and ROTI in Greenland and South America sectors, where 36 GNSS stations are localized in Greenland (**upper panels**) and 335 GNSS stations are situated in South America (**bottom panels**). Percentage of GNSS stations where (**a,b,e,f**) 3D-RMS \(\geqslant\) 3 cm; (**c,d,g,h**) maximum 3D position \(\geqslant\) 10 cm; (**a,c,e,g**) ROTI \(\geqslant\) 0.25 TECu/min; and (**b,d,f,h**) ROTI \(\geqslant\) 0.50 TECu/min. Percentage of GNSS stations meeting 3D-RMS (blue bars); maximum 3D positioning error (light blue bars); ROTI (orange bars); 3D-RMS and ROTI (green bars); and maximum 3D positioning error and ROTI (light green bars) values. Figure 8 presents the results of ionospheric TEC of 12 stations from among the 24 selected GNSS stations for the eclipse day (VTECe), the reference days (\(\overline{VTEC}\)), and the final results of DVTEC [%]. The vertical blue shaded region between P1 time and P4 time, with GE time (brown dotted line). The vertical yellow shaded region between C1 time and C4 time, with MOT (black dotted line). Each plot is shown between 5 and 23 UT. The maximum reduction values of TEC for each station are indicated in Table 1 (\(\tau=1\) to 288 min, and A[%]\(=-65\) to \(-27\)%). This eclipse occurred during the morning at most of the selected stations but took place in the afternoon at five stations (NYA1, TRO1, SVTL, TIXI, MAG0, YAKT). The Sun's activity became stronger around noon and the clear TEC reduction during the eclipse can be observed. The stations that are near the path of the annular eclipse at 350 km altitude and the east coast of Greenland reached lower values of DVTEC [%] \(\sim-55\)% than the stations with the annular eclipse at the surface level DVTEC [%] \(\sim-40\)%. Figure 8 shows the ionospheric TEC changes for 12 of the 24 GNSS stations presented in Table 1. The TEC disturbance lasted longer at the GNSS stations located in South America and the Lesser Antilles (CN00, LMMF, CN57, BOAV, PIFL, MSBL). In these GNSS stations, the ionospheric effect caused by the eclipse started at \(\sim\)8.5-9 UT and ended \(\sim\)18-21 UT (\(\Delta T>10\) h). The ionospheric response is similar in BOAV and MSBL stations where A[%] \(\sim-30\)%. In MAG0, TIXI, and YAKT stations, we observe a TEC depletion during the eclipse time window, but it is not as noticeable as in the other cases.