MCD is a database of atmospheric statistics compiled from Global Climate Model (GCM) numerical simulation of Martian atmosphere (<a href=http://www-mars.lmd.jussieu.fr>http://www-mars.lmd.jussieu.fr</a>). The GCM computes in 3D the atmospheric circulation and climate taking into account radiative transfer through the gaseous atmospheres and the dust and ice aerosols, includes a representation of the CO2 ice condensation and sublimation on the ground and in the atmosphere, simulates the water cycle (with modelling of cloud microphysics), the dust multisize particle transport, the atmospheric composition controlled by the photochemistry and the local non-condensible gas enrichment and depletion induced by CO2 condensation and sublimation, and has been extended into the thermosphere and to model ionospheric processes (due to chemistry). The database extends up to exobase (the top of the thermosphere, roughly at 300km in altitude); in addition to statistics on temperature, wind, pressure, radiative fluxes, it provides data such as atmospheric composition (including dust water vapor and ice content) and make use of 'dust and Extreme Ultra Violet (EUV) scenarios' to represent the variation of dust in the atmosphere and solar EUV conditions. User Manual of the service : <a href=http://vo.lmd.jussieu.fr:8080/MCD_VESPA_service_user_manual.pdf>User Manual of the service </a> .
"The growth of the Tharsis volcanic complex on Mars during
Noachian/Hesperian era induced a reorientation of the spin axis of the
planet (true polar wander). This service gives access to a map of Mars
topography before Tharsis formation (Early Noachian) and a map of Mars
topography before true polar wander (Late Noachian/Early Esperian),
from the model described in Bouley, S., Baratoux, D., Matsuyama, I. et
al. Late Tharsis formation and implications for early Mars. Nature
531, 344â347 (2016). https://doi.org/10.1038/nature17171 ."
The database contains profiles of atmospheric CO2 density and
temperature derived thereof, and ozone concentration profiles, all
derived from the first year(s) of SPICAM UV stellar occultation
observations (Forget et al. 2009, Lebonnois et al. 2006). The database
also includes the full dataset of four Martian years of aerosol
extinction profiles from SPICAM UV solar occultations (Määttänen et
al. 2013).
