Abstract:The evolution of the martian atmosphere and its H 2 O inventory can be divided into early and late evolutionary epochs. Volatiles such as H 2 O and CO 2 could have built up a dense water vapour dominated H 2 O/CO 2 steam atmosphere during the early impact and magma ocean solidification period. Due to the high activity of the young Sun, Mars' atmosphere experienced soft X-ray and EUV-driven hydrodynamic blowoff during the early Noachian, which could have powered the loss of an outgassed initial steam atmosphere… Show more
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