Minimum estimates of the amount and timing of gases released into the martian atmosphere from volcanic eruptions

作者：Craddock Robert A^*; Greeley Ronald

来源：Icarus, 2009, 204(2): 512-526.

DOI：10.1016/j.icarus.2009.07.026

• Mars
• Volcanism

Volcanism has been a major process during most of the geologic history of Mars. Based on data collected from terrestrial basaltic eruptions, we assume that the volatile content of martian lavas was typically similar to 0.5 wt.% water, similar to 0.7 wt.% carbon dioxide, similar to 0.14 wt.% sulfur dioxide, and contained several other important volatile constituents. From the geologic record of volcanism on Mars we find that during the late Noachian and through the Amazonian volcanic degassing contributed similar to 0.8 bar to the martian atmosphere. Because most of the outgassing consisted of greenhouse gases (i.e., CO2 and SO2 warmer surface temperatures resulting from volcanic eruptions may have been possible. Our estimates suggest that similar to 1.1 X 10(21) g (similar to 8 +/- 1 m m(-2)) of juvenile water were released by volcanism; slightly more than half the amount contained in the north polar cap and atmosphere. Estimates for released CO2 (1.6 x 10(21) g) suggests that a large reservoir of carbon dioxide is adsorbed in the martian regolith or alternatively similar to 300 cm cm(-2) of carbonates may have formed, although these materials would not occur readily in the presence of excess SO2. UP to similar to 120 cm cm(-2) (2.2 x 10(20) g) of acid rain (H2SO4) may have precipitated onto the martian surface as the result of SO2 degassing. The hydrogen flux resulting from volcanic outgassing may help explain the martian atmospheric D/H ratio. The amount of outgassed nitrogen (similar to 1.3 mbar) may also be capable of explaining the martian atmospheric N-15/N-14 ratio. Minor gas constituents (HF, HCl, and H2S) could have formed hydroxyl salts on the surface resulting in the physical weathering of geologic materials. The amount of hydrogen fluoride emitted (1.82 x 10(18) g) could be capable of dissolving a global layer of quartz sand similar to 5 mm thick, possibly explaining why this mineral has not been positively identified in spectral observations. The estimates of volcanic outgassing presented here will be useful in understanding how the martian atmosphere evolved over time. Published by Elsevier Inc.

• 出版日期2009-12