Carbon sequestration on Mars

On Earth, carbon sequestration in geologic units plays an important role in the carbon cycle, scrubbing CO2 from the atmosphere for long-term storage. While carbonate is identified in low abundances within the dust and soils of Mars, at < 1 wt% in select meteorites, and in limited outcrops, no massive carbonate rock reservoir on Mars has been identified to date. Here, we investigate the largest exposed carbonate-bearing rock unit, the Nili Fossae plains, combining spectral, thermophysical, and morphological analyses to evaluate the timing and carbon sequestration potential of rocks on Mars. We find that the olivine-enriched (similar to 20%-25%) basalts have been altered, by low-temperature in situ carbonation processes, to at most similar to 20% Fe-Mg carbonate, thus limiting carbon sequestration in the Nili Fossae region to similar to 0.25-12 mbar of CO2 during the late Noachian-early Hesperian, before or concurrent with valley network formation. While this is large compared to modern-day CO2 reservoirs, the lack of additional, comparably sized post-late Noachian carbonate-bearing deposits on Mars indicates ineffective carbon sequestration in rock units over the past similar to 3.7 b.y. This implies a thin atmosphere (less than or similar to 500 mbar) during valley network formation, extensive post-Noachian atmospheric loss to space, or diffuse, deep sequestration by a yet-to-be understood process. In stark contrast to Earth's biologically mediated crust: atmosphere carbon reservoir ratio of similar to 10(4)-10(5), Mars' ratio is a mere similar to 10-10(3), even if buried pre-Noachian crust holds multiple bars.