## 6 Summary and Concluding Remarks
Moderate to intense amplitude scintillations were triggered by conspicuous increase in ionization as observed through unusually high TEC values at the auroral latitudes. This confirmed the theoretical prerequisite of sufficient background TEC for E-field variations associated with precipitation to form electron density irregularities with scale sizes of the order of the first Fresnel radius. 4. The physical processes triggering amplitude scintillations at high and low latitudes are similar. However, since the ionosphere-magnetosphere-solar wind coupling acts in different ways in the two regions, the conditions necessary for the observation of amplitude scintillations at high latitudes are high levels of ionization and a strong plasma dynamics driven by fast oscillations in \(B_{\rm z,IMF}\) (of the order of ten minutes) resulting in geomagnetic storms, which typically occur during high solar activity. The characterization of the plasma conditions at high latitudes during geomagnetic storms, derived from this work, is propaedeutic to the characterization of the electromagnetic field near and inside the auroral oval and at higher latitudes. Such characterization could be benefit the calibration of instruments on board the China Seismo-Electromagnetic Satellite CSES-02 to facilitate collection of calibrated data at high latitudes. G.D., conceptualization, writing--original draft preparation, formal analysis and methodology, and investigation; M.P. ([PERSON]), writing--review and editing, validation and supervision; A.P., writing--review and editing, investigation; I.C., validation, writing--review and editing; P.D.M., writing--review and editing, investigation; R.T., writing--review and editing, and investigation; M.P. ([PERSON]), writing--review and editing; L.A., validation, writing--review and editing; P.C., data curation, and writing--review and editing; P.U., project administration, and writing--review and editing. All authors have read and agreed to the published version of the manuscript. This research received no external funding. **Data Availability Statement:** GNSS data from the Septentrio PolaRoS ISMRs located at Concordia station and SANAE IV base can be obtained from the eSWua website (www.eswua.ingv.it, accessed on 21 June 2021) doi.org/10.13127/. The IMF and solar wind data are provided by the NASA OMNIWeb service ([[http://omniweb.gsfc.nasa.gov](http://omniweb.gsfc.nasa.gov)]([http://omniweb.gsfc.nasa.gov](http://omniweb.gsfc.nasa.gov)), accessed on 21 June 2021). The _AE_, _AU_ and _AL_ indices were obtained from the World Data Center for Geomagnetism at Kyoto University ([[http://wdc.kugi.kyoto-u.ac.jp/](http://wdc.kugi.kyoto-u.ac.jp/)]([http://wdc.kugi.kyoto-u.ac.jp/](http://wdc.kugi.kyoto-u.ac.jp/)), accessed on 21 June 2021). The GPS TEC data used to construct TEC maps can be obtained through the UNAVCO Data Center ([[https://www.unavco.org/data/gps-gnss/gpss-gnss.html](https://www.unavco.org/data/gps-gnss/gpss-gnss.html)]([https://www.unavco.org/data/gps-gnss/gpss-gnss.html](https://www.unavco.org/data/gps-gnss/gpss-gnss.html)), accessed on 21 June 2021). The Special Sensor Ultraviolet Spectrographic Imager (SSUSI) data are available and documented at [[https://ssusi.huapl.edu](https://ssusi.huapl.edu)]([https://ssusi.huapl.edu](https://ssusi.huapl.edu)), accessed on 21 June 2021. The SSUSI Principal Investigator is Dr. [PERSON]. Swarm data are provided by the European Space Agency upon registration ([[https://earthes.in/web/guest/swarm/data-access/](https://earthes.in/web/guest/swarm/data-access/)]([https://earthes.in/web/guest/swarm/data-access/](https://earthes.in/web/guest/swarm/data-access/)), accessed on 21 June 2021).