This study tests a recent suggestion that multi-month soft X-ray emissions from supernovae can destroy planetary ozone layers. To test this, we assume a year-long solar flare and evaluate the production of nitric oxide in the upper atmosphere and its transport down to the stratosphere. Our results suggest widespread catalytic destruction of ozone; however, these effects are limited to the upper edge of the ozone layer (near 40 km). Thus, the total column is only slightly affected (1–2 %).

In previous works, we found Euler potentials for the combined magnetic field of Earth's dipole, field-aligned currents, ring currents, and magnetopause surface currents (represented by Dungey's term) in the magnetosphere. The determination of shell currents is difficult.

Comparisons of wind measurements using two different techniques (ground-based radar and satellite) in Brazil during 2006 were made in order to point out the advantages of each instrument for studies in the mesosphere and upper thermosphere. (i) For short-period variations, the measurements of the satellite were more advantageous. (ii) The monthly climatology using the radar was more appropriate. (iii) For long periods (longer than a few months), both instruments responded satisfactorily.

We study how well the F10.7 and F30 solar radio fluxes have represented solar energy input in the thermosphere in the last 60 years. We found that increased saturation of radio fluxes at recent solar minima leads to an overestimation of solar energy, which changes the relation between thermospheric parameters and F10.7, but this is not an issue for F30 because of a relative increase in F30 with respect to F10.7. This explains why F30 has been found to represent solar energy better than F10.7.

The boundary of Earth's magnetic field, the magnetopause, deflects and reacts to the solar wind, the energetic particles emanating from the Sun. We find that certain types of solar wind favour the occurrence of deviations between the magnetopause locations observed by spacecraft and those predicted by models. In addition, the turbulent region in front of the magnetopause, the foreshock, has a large influence on the location of the magnetopause and thus on the accuracy of the model predictions.

We analyzed the average magnetopause position influenced by solar winds and interplanetary magnetic field (IMF) using data from the Time History of Events and Macroscale Interactions during Substorms (THEMIS), Radiation Belt Storm Probes (RBSP), and Magnetospheric Multiscale (MMS) mission from 2016–2020. Minimal movement occurred during substorm phases. The magnetopause moved to its closest inward position during the growth phase and relaxed from peak to recovery as in Shue's model.