TY - JOUR
T1 - Carbon sequestration on Mars
AU - Edwards, Christopher S.
AU - Ehlmann, Bethany L.
N1 - Publisher Copyright:
© 2015 Geological Society of America.
PY - 2015/10/1
Y1 - 2015/10/1
N2 - 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 (~20%-25%) basalts have been altered, by low-temperature in situ carbonation processes, to at most ~20% Fe-Mg carbonate, thus limiting carbon sequestration in the Nili Fossae region 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 ~3.7 b.y. This implies a thin atmosphere (≲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 ~104-105, Mars' ratio is a mere ~10-103, even if buried pre-Noachian crust holds multiple bars.
AB - 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 (~20%-25%) basalts have been altered, by low-temperature in situ carbonation processes, to at most ~20% Fe-Mg carbonate, thus limiting carbon sequestration in the Nili Fossae region 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 ~3.7 b.y. This implies a thin atmosphere (≲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 ~104-105, Mars' ratio is a mere ~10-103, even if buried pre-Noachian crust holds multiple bars.
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U2 - 10.1130/G36983.1
DO - 10.1130/G36983.1
M3 - Article
AN - SCOPUS:84980318128
SN - 0091-7613
VL - 43
SP - 863
EP - 866
JO - Geology
JF - Geology
IS - 10
ER -