A5048315263- Astro and Planetary Science
- Planetary Science and Exploration
- Spacecraft and Cryogenic Technologies
- Ion-surface interactions and analysis
- Space exploration and regulation
- Solar and Space Plasma Dynamics
Centre National de la Recherche Scientifique
2023-2024
Laboratoire atmosphères, milieux, observations spatiales
2023-2024
Laboratoire Printemps
2023-2024
Sorbonne Université
2023
Abstract The surfaces of airless planetary bodies, such as the Moon or Mercury, are covered with regoliths, which interact solar wind. protons can either be absorbed by surface neutralized and reflected hydrogen energetic neutral atoms (ENAs). ENA flux is thought to depend mostly on structure upper regolith layer. By using a model combining Monte Carlo approach describe proton’s journey through lunar molecular dynamics characterize its interactions regolith’s grains, we highlight roughness...
Martian ionosphere has a stratified structure with two main layers in its electron density profile (Ne). The primary layer (M2 layer) is formed by solar EUV radiation (~20-90 nm) and peak at around 120-140 km altitude of ~1011 m-3. second (M1 occurs lower ~109 m-3 X-ray impact ionization. densities the altitudes which these peaks occur vary space weather activities. Radio Occultation (RO) experiments provide vertical profiles that span entire ionosphere. Therefore, RO are ideal for...
Abstract Mercury's surface undergoes large temperature gradients between day and night, which repeats periodically over the same longitudes due to its 3:2 spin‐orbit resonance. This effect combined with orbit's eccentricity, creates hot cold geographic longitudes. The planet is covered a highly porous regolith, allowing exospheric atoms diffuse in depth. By using 1‐D diffusion model, we studied subsurface precipitation of gas understand retention. work identifies as favorable regions form...