A5079416959- Astro and Planetary Science
- Planetary Science and Exploration
- Space Exploration and Technology
- Solar and Space Plasma Dynamics
- Atmospheric Ozone and Climate
- Stellar, planetary, and galactic studies
- Astrophysics and Star Formation Studies
- Geology and Paleoclimatology Research
- Isotope Analysis in Ecology
- Geomagnetism and Paleomagnetism Studies
- Atmospheric aerosols and clouds
- Spacecraft and Cryogenic Technologies
- Scientific Research and Discoveries
- Atmospheric chemistry and aerosols
- Ionosphere and magnetosphere dynamics
- Methane Hydrates and Related Phenomena
- Spacecraft Design and Technology
- Aeolian processes and effects
- French Urban and Social Studies
- Spectroscopy and Laser Applications
- Calibration and Measurement Techniques
- Diverse Cultural and Historical Studies
- Atmospheric and Environmental Gas Dynamics
- Space Satellite Systems and Control
- Laser-induced spectroscopy and plasma
Université de Reims Champagne-Ardenne
2015-2024
Centre National de la Recherche Scientifique
2015-2024
Groupe de Spectrométrie Moléculaire et Atmosphérique
2015-2024
Instituto Nacional de Técnica Aeroespacial
2023
Sorbonne Université
1993-2022
Université de Versailles Saint-Quentin-en-Yvelines
2003-2022
Observatoire de Paris
1995-2022
Laboratoire atmosphères, milieux, observations spatiales
2010-2022
Université Paris-Saclay
2022
Laboratoire de Météorologie Dynamique
1993-2022
In this paper, we present the results obtained by general circulation model developed at Laboratoire de Météorologie Dynamique which has been used to simulate Martian hydrological cycle. Our model, employs a simplified cloud scheme, reproduces observed water cycle with unprecedented agreement. The modeled seasonal evolution of cloudiness, also compares well data, is described in terms meteorological phenomena that control distribution. Whereas formation tropical region from changes...
Clouds have been observed recently on Titan, through the thick haze, using near-infrared spectroscopy and images near south pole in temperate regions 40 degrees S. Recent telescope Cassini orbiter observations are now providing an insight into cloud climatology. To study clouds, we developed a general circulation model of Titan that includes microphysics. We identify explain formation several types ethane methane including polar clouds sporadic especially at summer hemisphere. The locations,...
This paper is intended as an introduction to several companion papers describing the results obtained by SPICAM instrument on board Mars Express orbiter. a lightweight (4.7 kg) UV‐IR dual spectrometer dedicated primarily study of atmosphere Mars. The IR and its are described in another paper. first perform stellar occultations at Mars, UV imaging (118–320 nm, resolution ∼1.5 intensified CCD detector) was designed obtain atmospheric vertical profiles occultation. wavelength range dictated...
Spectra from Cassini's Visual and Infrared Mapping Spectrometer reveal the presence of a vast tropospheric cloud on Titan at latitudes 51 degrees to 68 north all longitudes observed (10 190 west). The derived characteristics indicate that this is composed ethane forms as result stratospheric subsidence particularly cool conditions near moon's pole. Preferential condensation ethane, perhaps ice, Titan's poles during winters may partially explain lack liquid oceans surface middle lower latitudes.
Abstract Observations of Titan through Cassini’s mission allowed Saturn’s moon’s stratospheric thermal structure and composition to be mapped over half a year. Seasonal variations revealed various unexplained phenomena, such as mechanisms within the polar vortex, evolution at high latitudes, impact enrichment in trace compounds during winter nights. We have developed Planetary Climate Model (Titan PCM)—an improved version IPSL Global (GCM)—including upgraded radiative transfer, now based on...
Abstract Observations of Titan have long revealed the presence seasonal cycles, including haze, clouds, and gases. The lack information on different processes that govern these cycles prevents us from understanding all phenomena taking place in Titan’s atmosphere. In this work, we survey exhaustively to understand their mechanisms, particular haze cloud a large part climate its surface. Planetary Climate Model (Titan PCM)—an upgraded version IPSL Global Model—incorporates microphysical model...
The smoggy stratosphere of Saturn's largest moon, Titan, veils its surface from view, except at narrow wavelengths centered 0.83, 0.94, 1.07, 1.28, 1.58, 2.0, 2.9, and 5.0 micrometers. We derived a spectrum Titan's within these “windows” detected features characteristic water ice. Therefore, despite the hundreds meters organic liquids solids hypothesized to exist on surface, icy bedrock lies extensively exposed.
Observations made by the SPICAM ultraviolet spectrometer on board Mars Express orbiter are presented. We focus several hundreds of atmospheric profiles which have been collected over 3/4 a Martian year making use stellar occultation technique. The typical structure haze possesses at least one discrete layer (60% all cases) standing an extended portion wherein opacity continuously increases down to surface. Differences morphology are, however, noted between observed near equator and...
In this paper we use a direct method which combines microphysics and photometric simulations of the Martian atmosphere. This approach allows us to reproduce vertical profiles light scattered by haze at limb Mars. Subsequent results are compared multiple‐color image provided Viking Orbiter camera. The “free parameters” our study related transport dust size distribution. A sensitivity has been conducted, encompassing relevant range parameters, in order obtain most satisfying multispectral...