- 1University of Turku, Department of Physics and Astronomy, Space Research Laboratory, Turku, Finland (annamaria.fedeli@utu.fi)
- 2Universidad de Alcalá, Space Research Group, Alcalá de Henares, Spain
- 3Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482, Potsdam, Germany
The Sun produces eruptive events that release energetic particles, such as protons and electrons, into the heliosphere. These solar energetic particles (SEPs) can reach exceptionally high energies and pose risks to satellite technology and astronauts in space, particularly those outside the protective shield of Earth’s magnetic field. Identifying the mechanisms that accelerate SEPs remains a significant challenge in current research, which hampers our ability to predict SEP events effectively. Even cutting-edge space missions such as Solar Orbiter and Parker Solar Probe often do not reach close enough distances to the Sun to make direct observations of the acceleration processes without interference from transport effects.
Analyzing the spectra of SEPs is essential for understanding the acceleration mechanisms involved, as different phenomena should exhibit unique spectral features. However, it is also recognized that transport effects can significantly alter these spectral shapes, and the intricacies of these processes are still not fully understood.
Our research targets a subset of SEPs, solar energetic electrons (SEEs). We utilize the advanced measurements obtained from the Energetic Particle Detector (EPD) onboard the Solar Orbiter spacecraft. EPD boasts unparalleled time and energy resolution, detecting energetic particles at a 1-second interval across energies ranging from suprathermal to relativistic. This data, combined with Solar Orbiter's varying proximity to the Sun, enables us to analyze SEE energy spectra with unprecedented detail and to better understand the transport effects involved.
In this study, we investigate the peak intensity spectra of the most intense SEE events recorded by Solar Orbiter/EPD at 43 keV from December 2020 to December 2022. The spectral characteristics are derived by fitting the spectra using various mathematical models. We will present the findings of our statistical analysis and compare them with previous research outcomes.
How to cite: Fedeli, A., Dresing, N., Vainio, R., Gieseler, J., Gómez Herrero, R., Espinosa Lara, F., Warmuth, A., and Schuller, F.: Spectral Analysis of the most intense Solar Energetic Electron Events Observed with Solar Orbiter from December 2020 to December 2022, EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-11505, https://doi.org/10.5194/egusphere-egu25-11505, 2025.
