## 3 Results
### TEC Changes and Ionospheric Maps Using GPS Stations
Figure 4: TEC maps during PSE2018 and its eclipse obscuration masks at 350 km ionospheric altitude (magenta lines) are presented. VTECe, \(\overline{VTEC}\), and DVTEC (%) are shown from left to right panels. Also, from top to bottom: P1 \(-\) 1 h (17.95 UT); P1 (18.93 UT); GE \(-\) 0.5 h (20.36 UT); GE (MPO \(\sim\)60% at 20.86 UT); GE + 0.5 h (21.36 UT); and P4 (22.79 UT). Figure 5: TEC maps during PSE2022 and its eclipse obscuration masks at 350 km ionospheric height (magenta lines) are shown. VTECe, \(\overline{VTEC}\), and DVTEC (%) are represented from left to right panels. Additionally, from top to bottom: P1 \(-\) 1 h (17.75 UT); P1 (18.75 UT); GE \(-\) 0.5 h (20.19 UT); GE (MPO \(\sim\)66% at 20.69 UT); GE + 0.5 h (21.19 UT); and P4 (22.63 UT). To study the effects of the PSEs, we chose six GPS stations located in Chile from among more than 390 GPS stations (see Figure 1), where five stations were under the partial region during both eclipses (LSCH, RCSD, IMCH, QLLN, XPLO, CSOM). Additionally, CYHT station was under the shadow of PSE2022, but it was not under the shadow of PSE2018. Table 1 contains more information about the eclipse conditions and the GPS stations to the ionospheric height of 350 km. Figure 6 shows the results of the TEC behavior of six selected GPS stations for the eclipse day (VTECe), the reference days (\(\overline{VTEC}\)), and the results of DVTEC (\(\%\)). We presented each plot between 12 UT and 24 UT. The brown dotted line presents GE time, and it is inside the light blue bar shading the region between P1 and P4. The black dotted line shows MOT; this line is inside the yellow bar between C1 and C4. Both eclipses occurred during the afternoon at six selected stations. We could clearly see the depletion of TEC during both eclipses. The six selected GPS stations had a recovery between 1.5 UT and 2.5 UT the day after both partial eclipses. Table 1 presents the minimum values of DVTEC for each of the six chosen GPS stations. On the days of PSE2018 and PSE2022, TEC with respect to the background TEC was \(-\)29% (\(\tau\)\(\sim\)7 to 43 min) and \(-\)50% (\(\tau\)\(\sim\)1 to 45 min), respectively. Although CHYT was not under the shadow of PSE2018, it had a noticeable minimum DVTEC (\(-\)28%, \(-\)6 TECu) at 22.65 UT, after 5 min that LSCH and after 107 min to GE time. Regarding PSE2022, CHYT did not show a clear TEC reduction near MOT at this station. LSCH had minimum DVTEC values greater than 0% and 0 TECu, but it showed an evident TEC depletion near MOT. We also estimated DVTEC using the first day before and the first day after the PSE2022 as reference days (DoYs 119 and 121 of 2022) due to the ionospheric behavior of the CHYT and LSCH stations, when we took the fifth day before and the fifth day after this eclipse as reference days (DoYs 115 and 125 of 2022), where DoYs 119 and 121 showed values of \(\text{Kp}>2^{+}\) and \(\text{Vsw}>450\) km (see Figure 2). On this occasion, the eclipse-induced effects were shown clearly at CHYT (DVTEC = 0%, \(-\)0.2 TECu, and \(\tau\) = 57 min) and LSCH (DVTEC = \(-\)25%, \(-\)4.1 TECu, and \(\tau\) = 32 min). The minimum DVTEC of CHYT occurred 5 min before the end of the partial eclipse in this station. From the ionospheric response due to the eclipse, using reference days DoYs 115 and 125 of 2022 with respect to employment as reference days DoYs 119 and 121 of 2022, we were able to observe that the GPS stations (IMCH, QLLN, and CSMO) located from \(\sim\)38\({}^{\circ}\)S geographic latitude to the south showed a difference in the minimum percentage of DVTEC of less than 11% and a difference of \(\tau\)\(\pm\) 5 min. The six selected GPS stations showed that the ionosphere was impacted by geomagnetic forcing on the days of the 2018 and 2022 eclipses. On the day of the 2018 eclipse, we can analyze the ionospheric changes from 16 UT.