Modeling aqueous perchlorate chemistries with applications to Mars

• Published in: Icarus (New York, N.Y. 1962) Vol. 207; no. 2; pp. 675 - 685
• Main Authors: Marion, G.M., Catling, D.C., Zahnle, K.J., Claire, M.W.
• Format: Journal Article
• Language: English
• Published: Amsterdam Elsevier Inc 01-06-2010; Elsevier
• Subjects: Astronomy; Calcite; Cosmochemistry; Earth, ocean, space; Estimates; Evaporation; Exact sciences and technology; Freezing; Geological processes; Liquids; Mars; Mars, Surface; Mathematical models; Mineralogy; Perchlorates; Soil (material); Solar system; Geological processes; Mars, Surface; Mineralogy; Cosmochemistry; Element abundance; Thermodynamic model; Modelling; XRD; Evaporation; Solar system; Low temperature
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2009.12.003

NASA’s Phoenix lander identified perchlorate and carbonate salts on Mars. Perchlorates are rare on Earth, and carbonates have largely been ignored on Mars following the discovery by NASA’s Mars Exploration Rovers of acidic precipitated minerals such as jarosite. In light of the Phoenix results, we updated the aqueous thermodynamic model FREZCHEM to include perchlorate chemistry. FREZCHEM models the Na–K–Mg–Ca–Fe(II)–Fe(III)–Al–H–Cl–Br–SO
4–NO
3–OH–HCO
3–CO
3–CO
2–O
2–CH
4–Si–H
2O system, with 95 solid phases. We added six perchlorate salts: NaClO
4·H
2O, NaClO
4·2H
2O, KClO
4, Mg(ClO
4)
2·6H
2O, Mg(ClO
4)
2·8H
2O, and Ca(ClO
4)
2·6H
2O. Modeled eutectic temperatures for Na, Mg, and Ca perchlorates ranged from 199
K (−74
°C) to 239
K (−34
°C) in agreement with experimental data.
We applied FREZCHEM to the average solution chemistry measured by the Wet Chemistry Laboratory (WCL) experiment at the Phoenix site when soil was added to water. FREZCHEM was used to estimate
SO
4
2
-
and alkalinity concentrations that were missing from the WCL data. The amount of
SO
4
2
-
is low compared to estimates from elemental abundance made by other studies on Mars. In the charge-balanced solution, the dominant cations were Mg
2+ and Na
+ and the dominant anions were
ClO
4
-
,
SO
4
2
-
, and alkalinity. The abundance of calcite measured at the Phoenix site has been used to infer that the soil may have been subject to liquid water in the past, albeit not necessarily locally; so we used FREZCHEM to evaporate (at 280.65
K) and freeze (from 280.65 to 213.15
K) the WCL-measured solution to provide insight into salts that may have been in the soil. Salts that precipitated under both evaporation and freezing were calcite, hydromagnesite, gypsum, KClO
4, and Mg(ClO
4)
2·8H
2O. Epsomite (MgSO
4·7H
2O) and NaClO
4·H
2O were favored by evaporation at temperatures >0
°C, while meridianite (MgSO
4·11H
2O), MgCl
2·12H
2O, and NaClO
4·2H
2O were favored at subzero temperatures. Incongruent melting of such highly hydrated salts could be responsible for vug formation elsewhere on Mars.
All K
+ precipitated as insoluble KClO
4 during both evaporation and freezing simulations, accounting for 15.8% of the total perchlorates. During evaporation, 35.8% of perchlorates precipitated with Na
+ and 48.4% with Mg
2+. During freezing, 58.4% precipitated with Na
+ and 24.8% with Mg
2+. Given its low eutectic temperature, the existence of Mg(ClO
4)
2 in either case allows for the possibility of liquid brines on Mars today. FREZCHEM also showed that Ca(ClO
4)
2 would likely not have precipitated at the Phoenix landing site due to the strong competing sinks for Ca as calcite and gypsum. Overall, these results help constrain the salt mineralogy of the soil. Differences between evaporites and cryogenites suggest ways to discriminate between evaporation and freezing during salt formation. Future efforts, such as sample return or in situ X-ray diffraction, may make such a determination possible.