Planetary Magnetic Fields and Solar Forcing: Implications for Atmospheric Evolution

By R. Lundin, H. Lammer, I. Ribas. 2007

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Atmospheric Escape and Evolution of Terrestrial Planets and Satellites (2008, background): “However, the present stellar sample analyzed by Wood et al. (2002, 2005), Lundin et al. (2007) is not large enough; therefore, many uncertainties regarding the early solar wind remain, and more observations of young solar-like G and K stars are needed to enhance our knowledge of stellar winds…”
What makes a planet habitable? (2009, background): “The ionopause location is controlled by the SWDP and little by the IMF, both of which are highly variable.”
The Sun in Time: Activity and Environment (2007, background): “Non-thermal escape is due to other processes in which energization and escape are related to microscopic non-thermal processes (e.g., particle acceleration; Lundin and Barabash 2004; Lundin et al. 2007).”
Outgassing History and Escape of the Martian Atmosphere and Water Inventory (2015, background): “Furthermore, the atmosphere can interact with crustal reservoirs by CO2 weathering and hydration processes, which occur at the surface and/or in the crust (e.g., Zent and Quinn 1995; Bandfield et al. 2003; Becker et al. 2003; Lundin et al. 2007; Lammer et al. 2008; Pham et al. 2009; Tian et al. 2009”