My first major academic project focused on the exploration of the influence of external factors such as space weather (including interactions with magnetic fields and particles of solar, galactic or extra-galactic origin) on atmospheric electrical processes and on the study of mechanisms responsible for two high-altitude atmospheric phenomena: red sprites and blue jets. To understand their generation, I analyzed the physical parameters of air and its composition at the observed altitudes, along with their emitted wavelengths, propagation patterns, lengths, and estimated total energies. I compared these observations with different theoretical models, considering both atmospheric electrification from lightning and the influence of cosmic rays (solar, galactic, or extragalactic) as potential sources. This was the topic of my BSc thesis, completed in 1999 at the Faculty of Physics, Bucharest University, under the supervision of Prof. Dr. Mircea V. Rusu.

For my master's thesis, which I completed in 2001 at Rheinische Friedrich-Wilhelms-Universität in Germany under the supervision of Prof. Dr. Peter L. Biermann, I researched the role of particle acceleration by supernova shocks, in both the interstellar medium and the enriched medium surrounding progenitor stars, in producing some of the most energetic observed cosmic rays. This research not only provided deeper insight into the origins and propagation mechanisms of high-energy cosmic ray abundances, but it also allowed me to gain valuable theoretical and computational astrophysics experience, preparing me for a future career in the field.

Upon returning to Romania, I was employed at the Astronomical Institute of the Romanian Academy, where I worked in the Solar Physics group. My research focused on solar activity and the study of active phenomena on the Sun and in the heliosphere. My most significant contribution involved developing a new method for identifying various solar activity manifestations in solar corona images. This method, which involves converting satellite images into phase space for analysis, was particularly sensitive in identifying the early stages of plasma motion and was successfully tested on SOHO/EIT images.

Additionally, I worked in the “Cosmology group” at the same institute, where I developed a new cosmological model with profound implications for understanding the Universe. Later, I joined the “Stellar Astrophysics and Planetary Systems” group, where I contributed to two major projects. The first was a space mission proposal to study the radio emissions generated in the atmospheres and magnetospheres of both solar and extrasolar planets using space-borne interferometric methods. The second involved developing a new, more precise method and instrumentation for conducting astronomical polarimetric observations.

My future plans include continuing to contribute to the advancement of the field, with the aim of deepening our understanding of the world and the Universe. In particular, I am interested in studying how changes in planetary magnetic field strength and orientation, such as during geomagnetic excursions or polarity reversals, might increase the power of geomagnetic storms at weaker solar activity and influence phenomena resulting from the interaction between space weather and the planetary atmospheric layers, biosphere, or lithosphere.