Photochemical Escape of Oxygen from Mars: Consequences for Climate History

R. Lillis (1) , Justin Deighan (2) , J. L. Fox (3) , S. Bougher (4) , Y. Lee (4) , M. Combi (4) , François Leblanc (5) , T. Cravens (6) , A. Rahmati (6) , H. Gröller (7) , B. Jakosky (2)

1 SSL - Space Sciences Laboratory [Berkeley]
2 LASP - Laboratory for Atmospheric and Space Physics [Boulder]
3 Department of Physics [Dayton]
4 AOSS - Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor]
5 HELIOS - LATMOS
6 Department of Physics and Astronomy [Lawrence Kansas]
7 LPL - Lunar and Planetary Laboratory [Tucson]

As well as this effort using in situ data, MAVEN can also constrain photochemical escape using remote sensing of the oxygen corona with the Imaging Ultraviolet Spectrograph (IUVS) [12, 13], the Solar Energetic Particle (SEP) instrument and the Solar Wind Ion Analyzer [14]. These multiple methods will eventually allow validation of photochemical escape from Mars and its dependence on solar and planetary conditions, enabling confident extrapolation back into the past

Domains: Sciences of the Universe [physics]

R. Lillis, Justin Deighan, J. L. Fox, S. Bougher, Y. Lee, et al.. Photochemical Escape of Oxygen from Mars: Consequences for Climate History. Fourth International Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life, Oct 2017, Flagstaff, Arizona, United States. pp.LPI Contribution No. 2014. ⟨insu-01664627⟩