Speaker
Description
Solar radio bursts (SRB), linked to intense solar events, are electromagnetic emissions resulting from instabilities (like the Langmuir decay instability) and wave couplings (such as the two-plasmon coalescence). They mainly appear at the plasma frequency ($\omega_p$) and its first harmonic ($2\omega_p$), $\omega_p$ being the electron plasma frequency at the source of the emission. Studying these processes provides new perspectives for the understanding of the solar wind and new opportunities for space weather forecast.
Since $2020$, experiments at LULI have shown that laser-plasma interactions can replicate most of these processes by generating Langmuir waves via the stimulated Raman instability. This results in the generation of electromagnetic waves at $\omega_p$ and $2\omega_p$ , similar to the emissions observed during solar bursts. In a forthcoming experiment, we will try to get closer to solar conditions, by introducing a magnetic field to mimic the one of the solar wind. Smilei PIC simulations will help us design and interpret this experiment.
In this poster, we will present the basic processes leading to SRB, how they are mimicked in our experiments, as well as the relevant plasma parameters for the two configurations (SRBs and experiment). We will then discuss the typical simulation setups we are envisioning to support our experiments and identify the processes responsible for electromagnetic plasmas at $\omega_p$ and its harmonics.
