Biology
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p43c1445t&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #P43C-1445
Biology
[1009] Geochemistry / Geochemical Modeling, [1011] Geochemistry / Thermodynamics, [1060] Geochemistry / Planetary Geochemistry, [5220] Planetary Sciences: Astrobiology / Hydrothermal Systems And Weathering On Other Planets
Scientific paper
The search for life on Mars includes the availability of liquid water, access to biogenic elements and an energy source. In the past, when water was more abundant on Mars, a source of energy may have been the limiting factor for potential life. Energy, either from photosynthesis or chemosynthesis, is required in order to drive metabolism. Potential martian organisms most likely took advantage of chemosynthetic reactions at and below the surface. Terrestrial chemolithoautotrophs, for example, thrive off of chemical disequilibrium that exists in many environments and use inorganic redox (reduction-oxidation) reactions to drive metabolism and create cellular biomass. The chemical disequilibrium of six different martian environments were modeled in this study and analyzed incorporating a range of water and rock compositions, water:rock mass ratios, atmospheric fugacities, pH, and temperatures. All of these models can be applied to specific sites on Mars including environments similar to Meridiani Planum and Gusev Crater. Both a mass transfer geochemical model of groundwater-basalt interaction and a mixing model of groundwater-hydrothermal fluid interaction were used to estimate hypothetical martian fluid compositions that results from mixing over the entire reaction path. By determining the overall Gibbs free energy yields for redox reactions in the H-O-C-S-Fe-Mn system, the amount of geochemical energy that was available for potential chemolithoautotrophic microorganisms was quantified and the amount of biomass that could have been sustained was estimated. The quantity of biomass that can be formed and supported within a system depends on energy availability, thus sites that have higher levels and fluxes of energy have greater potential to support life. Results show that iron- and sulfur-oxidation reactions would have been the most favorable redox reactions in aqueous systems where groundwater and rock interacted at or near the surface. These types of reactions could have supported between 0.05 and 1.0 grams (dry weight) of biomass per mole of iron or sulfur. The hydrothermal environments would have had numerous redox reactions in the H-O-C-S-Fe-Mn system that could have provided sufficient metabolic energy for potential microorganisms. Methanotrophy, for example, provides the greatest amount of energy at ~760 kJ per mole of methane, which is equivalent to 0.6 grams (dry weight) of biomass. Additional results show that varying the amount of CO2 in the martian atmosphere or adjusting the water:rock ratios has little effect on the resulting Gibbs free energies. The martian values that are reported for available free energy in this study are similar to values that have been calculated for terrestrial systems in hydrothermal settings in which life is known to be abundant. In summary, the models indicate that martian aqueous environments were likely to have been habitable at a wide range of conditions when liquid water was more abundant and would have been able to supply a large amount of energy for potential organisms.
Jakosky Bruce M.
Tierney L. L.
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