Atmospheric Escape and Evolution of Terrestrial Planets and Satellites

By H. Lammer, J. Kasting, E. Chassefière, Robert E. Johnson, Y. Kulikov, F. Tian. 2008

258 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/caa80ffebbb746afa952e567afe2d53848bc9bab

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In Astronomy and Astrophysics

Citations in the corpus

Atmospheric Escape and the Evolution of Close-In Exoplanets (2018, background): “This available energy means that unlike Solar-System planets, where atmospheric escape is vital for shaping the chemical evolution of a planet’s atmosphere (e.g. Lammer et al. 2008), in the context of closein exoplanets, atmospheric escape can affect the evolution of a planet’s bulk composition.”
What makes a planet habitable? (2009, background): “As shown in Table 8 the soft X-ray and EUV radiation of an active star is responsible for heating and expansion of the upper atmospheres (Kulikov et al. 2006, 2007; Lammer et al. 2008; Tian et al. 2008).”
Outgassing History and Escape of the Martian Atmosphere and Water Inventory (2015, background): “Although the previous sections have shown that due to the high EUV flux of the young Sun, atmospheric escape models do not favor a dense CO2 atmosphere during the first Gyr, we now investigate possible effects of the late heavy bombardment (LHB) period.”
Origin of acidic surface waters and the evolution of atmospheric chemistry on early Mars (2010, background): “7 Gyr ago, significantly later into martian geologic history than is generally though”
How Hospitable Are Space Weather Affected Habitable Zones? The Role of Ion Escape (2017, unknown): “Hydrogen, as the lightest component, escapes more readily than any other species by this mechanism ( Lammer et al. 2008; Tian et al. 2008 ) .”
Loss of the Martian atmosphere to space: Present-day loss rates determined from MAVEN observations and integrated loss through time (2018, background): “When recombination occurs above the exobase, such that the upward-moving atom is not likely to be backscattered or slowed below escape energy by subsequent collisions, it will escape to space (e.g., Lillis et al., 2017; Fox and Hac, 2009; Lammer et al., 2008; Groller et al., 2014).”
A theoretical framework for volcanic degassing chemistry in a comparative planetology perspective and implications for planetary atmospheres (2014, background): “4 In addition to heliocentric distance, one obvious possibility to explain such a diversity is to relate it with long gone processes, such as changes in the luminosity of the Sun, chondritic bombardments, intensity of the magnetic field, solar wind erosion, each of which has clearly played a role on”
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds. (2012, background): “5 Gyr are below a few hundreds of millibars (Leblanc and Johnson, 2002; Lammer et al., 2008; Lammer, 2010).”