## 1 Introduction  
The ionospheric TEC changes can be provoked by some sources, such as solar flares, geomagnetic storms, solar eclipses, solar terminators, tropical cyclones, thunderstorms/ lightning, volcanic eruptions, earthquakes, tsunamis, and rocket launches, among others [1, 2]. These ionospheric disturbance sources can cause blackouts in radio signals and are an important problem for satellite communication and radiomavigation systems [2]. Solar eclipses provide a unique opportunity to investigate atmospheric and ionospheric processes from the Earth's surface to the topside ionosphere during the fast sunlight-umbra transitions and vice versa. During solar eclipses, solar radiation is attenuated because it is partially blocked by the Moon. Consequently, the sudden decreases in photo-ionization and photo-electron heating of solar extreme ultraviolets (EUVs) affect all the ionospheric layers [3]. This results in the loss of plasma and a local drop in electron density (\(N_{e}\)) dominating the output rate on an eclipse day relative to a regular day. The total electron content (TEC in TECu, where 1 TECu = \(10^{16}\) el/m\({}^{2}\)) is a measure of \(N_{e}\) in the ionosphere integrated along the line of sight; therefore, it provides accurate information about ionization behavior. During eclipses, the TEC fluctuates and can be characterized by the amplitude as differential TEC (in TECu and/or %), which usually has a reduction; delay value (\(\tau\) in min) relative to the maximum obscuration time (MOT) of the eclipse; and duration (\(\Delta T\) in hours) of the disturbance [1]. TEC can be estimated via a radio link between Earth and space. The Global Navigation Satellite System (GNSS) is the most widely used communication system for estimating TEC in the ionosphere. Therefore, we use the Global Positioning System (GPS) in this work, which is one of the constellations of satellites that make up GNSS. The solar eclipse-induced effects on the ionosphere are not simply local, but can even influence areas outside the eclipse's shadow. These effects may be caused by the transfer of hemisphere magnetic conjugates, changes in the equatorial vertical E \(\times\) B drift, the development of a disturbance dynamo, and atmospheric gravity waves (AGWs) that generate traveling ionospheric disturbances (TIDs) and/or traveling atmospheric disturbances (TADs) [4; 5; 6; 7; 8; 9; 10; 11; 12; 13; 14; 15; 16]. The supersonic moving shadow of solar eclipses on Earth's atmosphere can cause AGWs. Furthermore, the existence of eclipse waves (AGWs, TADs, and TIDs) affects a number of systems, including radiocommunication, radionavigation, and geolocalization. Ionospheric effects during high-latitude eclipses are driven by intense ionosphere-magnetosphere coupling, particularly during high levels of geomagnetic activity [17; 18; 19]; while ionospheric effects during low-latitude eclipses are influenced by electrodynamics processes associated with the equatorial ionization anomaly (EIA) [20; 21]. The equatorial vertical E \(\times\) B drift, which induces plasma transfer from the magnetic equator to the crest area and decreases strongly during solar eclipses, as has been seen, for example, during the 4 October 1995 and the 9 March 1997 solar eclipses [22]. It has been seen that the EIA source effect is frequently suppressed during Sun-Earth-Moon alignments (full moon, new moon, and eclipse), even with evidence of equatorial counter-electrojets during solstices [23; 24; 25; 26]. On the other hand, depending on the geometric configuration of the eclipse and season of occurrence, it can increase or decrease the EIA crests separately, generating asymmetry. Additionally, [PERSON] et al. [27] showed a summary of current studies that found EIA crests decreasing during solar eclipse occurrences, where TEC decrease was between \(-50\%\) and \(-20\%\) in comparison to the background ionosphere. In contrast, some authors found TEC increases around the EIA (e.g., [28; 29; 30; 31]). For instance, [PERSON] et al.