45th Lunar and Planetary Science Conference (2014) 2543.pdf Modeling and Mineralogical Analyses of Potential Martian Chloride Brines. P. E. Martin, M. S. Gilmore, and J. P. Greenwood, Dept. of Earth and Environmental Sciences, Wesleyan University, Middletown, CT 06459 (pemar-
[email protected]) Introduction: The discovery of salts in the Viking ined using X-ray diffraction (XRD) and VNIR (0.35- soils prompted investigation into the stability and 2.5 µm) spectra collected by an ASD FR spectrometer. composition of theoretical martian brines [e.g., 1, 2]. Results: The evaporation of the brines generally Such brines may be metastable on modern Mars and took place over a two to five week period, which de- have been invoked in the formation of modern fluvial pended on the concentration of the brine and its com- features on Mars such as gullies and slope lineae [3-5]. nposition (i.e. more deliquescent solutions took more The evaporation of such brines should result in the time). CLM, and SDJ remained in solution and were formation of mineral deposits that could potentially be not analyzed further. TPR did not fully evaporate, but recognized in visible-near-infrared (VNIR) spectra crystals formed, and these were harvested and put in a collected by the CRISM instrument on the Mars Re- dessicator for analysis. Many samples (MKS, KS, connaisance Orbiter, although this has not yet occurred TB1, TPR, TB5, CV2, CV3) contained residual water, [3]. In this work, we measure the VNIR spectra of ana- possibly due to deliquescence. MKS, KS, and TB1 logue chloride-rich martian evaporite assemblages in were analyzed with the water still present, while TPR, an attempt to better understand which minerals are TB5, CV2, and CV3, were placed in a dessicator to detectable using CRISM and how well VNIR spectra facilitate evaporation before analysis.