Thermal escape of carbon from the early Martian atmosphere

By F. Tian, J. Kasting, S. Solomon. 2009

142 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/ece5bc3edfba1dc333ec5a53fbfc2cec83ac88d2

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In Astronomy and Astrophysics

Citations in the corpus

Loss of the Martian atmosphere to space: Present-day loss rates determined from MAVEN observations and integrated loss through time (2018, background): “(Tian et al., 2009); this would have increased the early loss of CO2 above that described here.”
Outgassing History and Escape of the Martian Atmosphere and Water Inventory (2015, methodology): “As shown by Tian et al. (2009) a hotter thermosphere leads to an expansion of the upper atmosphere and thus more extended coronae.”
The Sample Analysis at Mars Investigation and Instrument Suite (2012, background): “For example, a recent hydrodynamic thermosphere-ionosphere model (Tian et al. 2009) predicts early Noachian massive CO2 loss resulting from the strong EUV flux present at that time giving rise to atmospheric conditions that would not support surface liquid water.”
Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, background): “…Sun’s EUV activity and related rotation history, Mars could have lost its magma ocean outgassed steam atmosphere early on (Erkaev et al. 2014), or may have kept several bar of CO2 at about 0.1 Gyr (Tian et al. 2009; Amerstorfer et al. 2017), if one assumes that the young Sun was a slow rotator.”
Origin of acidic surface waters and the evolution of atmospheric chemistry on early Mars (2010, result): “Given the absence of a complementary electron-rich reservoir preserved in the ancient crust (for example, significant sulphide mineral or reduced C-bearing deposits), these results may indicate the operation of H 2 -escape processes such as hydrodynamic escap”
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds. (2012, background): “3. Which atmosphere for early Mars? By scaling the Earth or Venus volatile inventory, one can estimate that the amount of CO2 broughtto Mars duringaccretion was probably larger than 10 bars. However, Tian et al. (2009) showed that the extremeultraviolet ﬂuxfromthe youngsun wa s so high that it would”
Updated global map of Martian valley networks and implications for climate and hydrologic processes (2010, background): “Tian et al.[2009] modeled loss from the early Martian atmosphere under the hypothesized strong EUV flux from the sun at that time.”
The Surface UV Environment on Planets Orbiting M Dwarfs: Implications for Prebiotic Chemistry and the Need for Experimental Follow-up (2017, background): “1= Ä)suggest thatits atmosphere would have been unstable to escape powered by higher XUV emission from the young Sun (Tian et al. 2009).”