## 3 Results
### TEC Changes and Ionospheric Maps Using GPS Stations  
Figures 4 and 5 show the summaries of ionospheric maps by comparing the eclipse (VTECe) and the reference days (\(\overline{VTEC}\)) for PSE2018 and PSE2022, respectively. Eclipse masks are represented from 5% obscuration at 350 km altitude (magenta lines). For both eclipses, we present some particular hours: P1 \(-\) 1 h, P1, GE \(-\) 0.5 h, GE, GE + 0.5 h, and P4. Figure 4 illustrates the ionospheric TEC behavior during PSE2018; where 17.95 UT (P1 \(-\) 1 h maps), 18.93 UT (P1 maps), 20.36 UT (GE \(-\) 0.5 h maps), 20.86 UT with MPO \(\sim\)60% (GE maps), 21.36 UT (GE + 0.5 h maps), and 22.79 UT (P4 maps). To see TEC maps from other hours, please go to Supplementary Materials Videos S1 and S2. From 16.85 UT, we could see that TEC is mostly positive relative to the background TEC (DVTEC \(\sim\)50%) between 30\({}^{\circ}\)S and 90\({}^{\circ}\)S, and it was \(\pm\)15% between 30\({}^{\circ}\)S and 0\({}^{\circ}\) latitude. This TEC enhancement can be clearly seen at 17.95 UT (P1 \(-\) 1 h maps). The P1 maps (\(\sim\)18.93 UT) show that the DVTEC value decreases slightly between 30\({}^{\circ}\)S and 90\({}^{\circ}\)S, where it was \(\sim\)20% in this southern South America region. At 19.50 UT, there is a decrease in TEC (DVTEC \(\sim\)\(-\)20%) in the Antarctica region between 45\({}^{\circ}\)W and 135\({}^{\circ}\)W longitude. At 20.15 UT, a notable TEC decrease begins around the southern EIA crest over South America around 30\({}^{\circ}\)S, 60\({}^{\circ}\)W. This TEC change continues to lower its value (DVTEC \(\sim\)\(-\)50%) and expand its region over South America as time passes. This phenomenon can be observed in the GE \(-\) 0.5 h (20.36 UT), GE (20.86 UT), GE + 0.5 h (21.36 UT), and P4 (22.79 UT) maps. From 20:50 UT, there is a shift in TEC decrease relative to the background TEC from the southeast (Antarctic sector) that passes through South Georgia and the South Sandwich Islands in the southern Atlantic Ocean and reaches southern South America at about 20.86 UT (GE maps, where MPO \(\sim\)60%). DVTEC remained positive over the studied sector of the Antarctic Peninsula until \(\sim\)20.65 UT. In the Antarctic sector, TEC is negative relative to background TEC, and the minimum DVTEC was \(\sim\)\(-\)40% at 20.65 UT. At about 20.86 UT (see GE maps), we see the DVTEC depletion move from southwest Antarctica to the northeast, and it reaches southern South America. Additionally, the recovery of TEC and some positive values of DVTEC appear over the Antarctic sector. About 22.80 UT (see P4 maps), we can observe the recovery of TEC in southern Chile and Argentina (up to 45\({}^{\circ}\)S latitude), but TEC depletion over South America persisted until after 24 UT. Moreover, after P4, the maximum DVTEC was \(>\)40% over the Antarctic region, similar to that before the first contact of the eclipse. Figure 5 is the same as Figure 4 but shows TEC variations during PSE2022. Figure 5 exhibits some particular hours: 17.75 UT (P1 \(-\) 1 h); 18.75 UT (P1); 20.19 UT (GE \(-\) 0.5 h); 20.69 UT (GE) with MPO 66%; 21.19 UT (GE + 0.5 h); and 22.63 UT (P4). At least before 16 UT, TEC enhancement was \(>\)20% relative to the background over South America (30\({}^{\circ}\)S to 60\({}^{\circ}\)S). This TEC enhancement is clearly illustrated on the P1 \(-\) 1 h and P1 maps. After P1, we could observe a decrease in TEC with \(<\)\(-\)10% along the Antarctic coasts between 60\({}^{\circ}\)W and 120\({}^{\circ}\)W. TEC decrease (DVTEC \(\sim\)\(-\)50%) reaches around Drake Passage (\(\sim\)60\({}^{\circ}\)S, \(\sim\)60\({}^{\circ}\)W) at 20.45 UT. At 20.70 UT, DVTEC had values of around \(-\)40% over southern South America and Antarctica (see GE + 0.5 h maps). The visible TEC decrease (DVTEC \(<\)\(-\)10%) reaches up to 30\({}^{\circ}\)S over South America. The improvement of TEC from the geomagnetic equator to 30\({}^{\circ}\)S latitude is reinforced around 21.20 UT, and it is maintained for at least 24 UT (P1 + 0.5 h and P4 maps).