Mars atmospheric escape and evolution; interaction with the solar wind

By E. Chassefière, François Leblanc. 2004

187 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/a1557c233a32d8e429d122829de2f1a3a5af5c02

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In Astronomy and Astrophysics

Citations in the corpus

The Climate of Early Mars (2016, background): “In contrast, escape processes occurring from the Hesperian onwards appear unambiguously ineffective: ion escape, plasma instability, sputtering and non-thermal processes combined could not have removed more than a few 100 mbar at most since 4 Ga (Chassefière & Leblanc 2004; Lammer et al. 2013).”
Origins of volatile elements (H, C, N, noble gases) on Earth and Mars in light of recent results from the ROSETTA cometary mission (2016, unknown): “Chassefière and Leblanc (2004) reviewed potential escape mechanisms that might have affected the atmosphere of Mars and concluded that (i) not a single process can account for the observations; and (ii) non-thermal processes are required and therefore might have affected different atoms/species at…”
Observation of the hydrogen corona with SPICAM on Mars Express (2008, background): “One obvious process leading to H escape to space is the thermal escape or Jeans escape (Chassefière and Leblanc, 2004) which has been estimated as being equal to 3.”
Atmospheric Escape and Evolution of Terrestrial Planets and Satellites (2008, methodology): “7 the history of the martian atmosphere can be divided into early and late evolutionary periods (e.g., Carr 1987; Zahnle et al. 1990; Carr 1996; Pepin 1994; Hutchins and Jakosky 1996; Chassefière and Leblanc 2004; Donahue 2004; Chassefière and Leblanc 2004).”
The Sun in Time: Activity and Environment (2007, background): “Non-thermal escape processes (of O) alone may explain the loss of a 12 – 15m Martian ocean during the past 3.5Gyrs (Lammer et al. 2003a; Chassefière and Leblanc 2004, and further references therein converging to similar numbers).”
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds. (2012, background): “(Chassefière and Leblanc, 2004). Up to now, only the presentday Mars ion loss by solar wind interaction has been measured, and found to be very small (Barabash et al., 2007). The possible loss of volatiles resulting from large impacts (Melosh and Vickery, 1989) is also difficult to model and constra”