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Improved general circulation models of the Martian atmosphere from the surface to above 80 km
We describe a set of two “new generation” general circulation models of the Martian atmosphere derived from the models we originally developed in the early 1990s. The two new models share the sameExpand
Global Mineralogical and Aqueous Mars History Derived from OMEGA/Mars Express Data
Global mineralogical mapping of Mars by the Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activité (OMEGA) instrument on the European Space Agency's Mars Express spacecraft provides newExpand
Warming early Mars with carbon dioxide clouds that scatter infrared radiation.
Model calculations show that the surface of early Mars could have been warmed through a scattering variant of the greenhouse effect, resulting from the ability of the carbon dioxide ice clouds to reflect the outgoing thermal radiation back to the surface. Expand
Increased insolation threshold for runaway greenhouse processes on Earth-like planets
A three-dimensional global climate model is used to show that the insolation threshold for the runaway greenhouse state to occur is about 375 W m−2, which is significantly higher than previously thought and has strong implications for the possibility of liquid water existing on Venus early in its history, and extends the size of the habitable zone around other stars. Expand
A climate database for Mars
A database of statistics which describe the climate and surface environment of Mars has been constructed directly on the basis of output from multiannual integrations of two general circulationExpand
3D climate modeling of close-in land planets: Circulation patterns, climate moist bistability and habitability
The inner edge of the classical habitable zone is often defined by the critical flux needed to trigger the runaway greenhouse instability. This 1D notion of a critical flux, however, may not be soExpand
Formation of Recent Martian Debris Flows by Melting of Near-Surface Ground Ice at High Obliquity
It is shown that these gullies on Mars may result from the melting of water ice in the top few meters of the martian subsurface at high obliquity, and that above-freezing temperatures can occur in the near surface of Mars, but are only predicted at latitudes and for slope orientations corresponding to where the gullies have been observed on Mars. Expand
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds.
On the basis of geological evidence, it is often stated that the early martian climate was warm enough for liquid water to flow on the surface thanks to the greenhouse effect of a thick atmosphere.Expand
Recent ice-rich deposits formed at high latitudes on Mars by sublimation of unstable equatorial ice during low obliquity
Using the ice accumulation rates estimated from global climate model simulations, it is shown that, over the past ten million years, large variations of Mars' obliquity have allowed the formation of such metres-thick, sedimentary layered deposits in high latitude and polar regions. Expand
Formation of Glaciers on Mars by Atmospheric Precipitation at High Obliquity
High-resolution climate simulations performed with a model designed to simulate the present-day Mars water cycle but assuming a 45° obliquity points to an atmospheric origin for the ice and reveals how precipitation could have formed glaciers on Mars. Expand