## 3 Results
### Ionospheric Behavior and TEC Maps
The 13.19 UT and 13.72 UT maps show another slight recovery of the ionospheric TEC in the North Atlantic and Greenland, as well as a TEC depletion over Russia. Moreover, TEC depletion was accentuated in the EIA crests over South America, where DVTEC[%] had values of less than \(-60\%\) (\(<\)\(-11\) TECu). It is shown that the effects lasted beyond the end of the eclipse. The 17.66 UT maps present the global recovery of the ionosphere a few hours after the end of the eclipse. These maps show a slight DTEC[%] enhancement in the center of the EIA form \(\sim\)\(-16\%\) to \(\sim\)10%. But the TEC depletion was \(\sim\)\(-20\%\) (\(-5\) to \(-3\) TECu) in the EIA crest over South America. The TEC behavior in the EIA crests was maintained until after 19.66 UT. On the other hand, DoY 162 had geomagnetic activity (see Section 2.5). Therefore, we checked if the DVTEC changes that we observed for the day of the eclipse were due to using DoY 162 as one of the reference days. We compute a new \(DVTEC_{t}\) (\(DVTECnew_{t}\), Equation (1)), and a new \(\overline{VTEC_{t}}\) by averaging the VTEC values at the same time of the day, \(t\), for the reference days, DoYs 159, 160, and 163. For each map, we used the map algebra (\(DVTEC_{t}-DVTECnew_{t}\)). The mean value ranged between \(-0.5\) and \(0.1\) TECu, with a standard deviation of less than \(0.7\) TECu (see Supplementary Materials, Figure S2, Table S1). Therefore, geomagnetic activity during the DoY 162 did not cause problems in the background to our ionospheric TEC results for the eclipse day. Ionospheric Behavior Using Swarm Satellite Measurements  
We also present ionospheric behavior using Swarm-A measurements (see Figure 4). We illustrate VTEC at 850 km altitude on DoY 161 compared to DoY 159 during three ascending passes of the Swarm-A satellite (\(\geqslant\)45\({}^{\circ}\)S, see Figure 4 (upper panels)). We selected the three Swarm-A satellite passes that best fit the eclipse region and eclipse time window. The first satellite pass (\(\sim\)8.50-9.20 UT) occurred after P1 time. The greatest ionospheric TEC degradation was \(-30^{\circ}\)S-\(30^{\circ}\)N (\(\sim\)\(-1.7\) TECu, \(-35\%\)). The second pass (\(\sim\)10.10-10.80 UT) was close to the GE time. As latitude increases, TEC decrease. The third satellite pass (\(\sim\)11.70-12.40 UT) was performed prior to P4 time (\(\sim\)\(-1.9\) TECu, \(-37\%\)). It is possible to see that TEC decrement was concentrated between 10 and \(30^{\circ}\)N (VTEC was close to \(\sim\)\(-1\) TECu, and \(\sim\)\(-30\%\)). Ionospheric TEC depletion was greatest in the 15-75\({}^{\circ}\)N region (\(\sim\)\(-2\) TECu, \(-45\%\)). Figure 4 (bottom panels) depict in situ \(N_{e}\) measurements made by Swarm-A Langmuir probe. Figure 4 (upper panels) show that VTEC behaves similarly to \(N_{e}\). We observed that \(N_{e}\) decrease was \(-46\%\) (\(-0.26\times 10^{5}\) e/cm\({}^{3}\)) at \(\sim\)8.86 UT in \(\sim\)\(1^{\circ}\)N; \(-55\%\) (\(-0.39\times 10^{5}\) e/cm\({}^{3}\)) at \(\sim\)10.62 UT in \(\sim\)\(50^{\circ}\)N; and \(-55\%\) (\(-0.72\times 10^{5}\) e/cm\({}^{3}\)) at \(\sim\)12.05 UT in \(\sim\)\(20^{\circ}\)N.