A Methane-Rich Early Mars: Implications for Habitability and the Emergence of Life

High levels of CH4 in Mars's early atmosphere may have played a significant role in determining whether or not the planet was habitable or suitable for the emergence of life. Via the coupling of radiative-convective and photochemical models, we investigate the nature of Mars's 4.0 Ga atmosphere, which is sourced primarily from CH4—not CO2—degassing. This is consistent with a mantle that does not reach the requisite pressure (24 GPa) and temperature (1900 K) for the silicate spinel-to-perovskite transition, which would oxidize the mantle thanks to ferrous iron's tendency to disproportionate to ferric iron in the presence of silicate perovskite (Dale et al., 2012; McCammon, 1997; Wadhwa, 2001; Wood et al., 2006). Impact degassing from chondritic material can also contribute substantial amounts of CH4 to the atmosphere (Schaefer and Fegley, 2007). A terrestrial world whose atmosphere is laden with CH4 would not drive the emergence of life according to the alkaline hydrothermal vent theory (e.g. Martin et al., 2008; Russell et al., 2014, 2010), which relies on the presence of copious CO2. However, CH4 will be oxidized as a result of photochemistry and hydrogen escape; if this process is efficient enough, there will be CO2 aplenty. On the other hand, if CH4 is converted to CO2 too efficiently, then early Mars may lose the greenhouse warming it needs to maintain liquid water at the surface. We use RC1D, a non-gray 1-D radiative-convective equilibrium model, to calculate the atmospheric thermal structure consistent with the radiative heating and cooling associated with the composition computed at each chemical model time step, the Sun's luminosity at that time, and global average insolation conditions. KINETICS, the Caltech/JPL chemistry transport model (e.g. Nair et al., 1994), determines the chemical makeup of the atmosphere, how effectively CH4 can be oxidized to CO2, and evaluate the synthesis of organic molecules in the atmosphere. The atmosphere is in vapor pressure equilibrium with an H2O ocean (Villanueva et al., 2015) or massive glaciation (Fastook and Head, 2015), losing hydrogen to space via hydrodynamic escape, and irradiated by the faint-young Sun. This study is a step towards a grander, more realistic model of early Mars that includes sulfur chemistry, atmospheric dust and haze, and aqueous chemistry.