The equatorial ionosphere over the Ecuadorian territory has not been previously studied, although there are some studies in other equatorial geographical positions, local research is required to characterize the ionospheric magnetoactive plasma in this region. In this study, for the first time in Ecuador, using pseudophase and pseudorange data from the satellite signals of the GPS system, detected at the Riobamba-Ecuador (RIOP) station, the Total Electronic Content (TEC) is estimated in the period between the years 1999 and 2019. The TEC values and their daily, weekly, monthly and annual variation are calculated and compared with the observed data of the IGS network (International GNSS Service). The fit of the observed series with the series of the dispersive model has a goodness of fit of 0.88, which is quite acceptable. The adjustment can be improved by incorporating data from new local stations, as well as instrumental errors and delays and in the received signals, all of which were not considered in the present work.

The James Webb Telescope (JWST), launched at the end of 2021, will permit the study of exoplanets’ atmospheres with an accuracy never obtained before. One of the most keenly anticipated science themes with JSWT data is the study of super-Earth type planets. There exist many questions about their interior and atmospheric composition as well as their evolution and possible migrations. In this work, we simulated transmission spectra of super-Earth type systems with the petitRADTRANS code and emission spectra of a M-type star with PySynphot. The primary transit observation is simulated with the MIRISim simulator working in the MIRI LRS-Slitless mode. We then obtained the transmission spectra of the planet using a code that we developed ourselves. Finally, we carried out the retrieval: first, in order to check the retrieval tool included in the petitRADTRANS code, we treated the original transmission spectrum. Second, the code is used with the spectrum obtained from the telescope simulator. The results found encourage us to compare them to results found when using other tools, with the hope of gaining precision in those results, in addition to working in a wider range of wavelengths.

In the present work, in order to estimate the semi-amplitude of the radial velocity, we evaluate the contribution of the Doppler beaming effect to the phase curves of the all confirmed extrasolar planets (2776, September 2019), observed so far by the Kepler telescope. By modeling the tiny photometric variations (reflection, ellipsoidal and Doppler beaming effects) of the light curves, we found that the best observational data are in close agreement with the theoretical and published values of the amplitudes only for exoplanets: KOI-13b and TrES-2b. The derived values for the radial velocity also are in good agreement with those published by some authors. Furthermore, we found it necessary to introduce a third harmonic (3Φ) contribution into the KOI-13b and HAT-P7b light curve models, in order to decrease the residuals.