Chloride-bearing deposits on Mars
Across the southern highlands of Mars, approximately 640 sites of chloride-bearing deposits have been identified using the Thermal Emission Imaging System (THEMIS). These isolated, irregularly-shaped patches (approximate size range of 0.33 – 1300 km2, with an average size of 24 km2) have been dated to the older geologic periods on Mars: Noachian (4.5 – 3.5 billion years ago) and Hesperian (3.5 – 2.9 billion years ago) periods. On Earth, chlorides are known to form through aqueous processes. Similar processes are expected to be responsible for the formation of chloride deposits on Mars. The finding of these deposits is significant in that it provides further evidence for the presence of surface or subsurface water in ancient Mars.
Importance of chlorides
Chlorides contain the anion Cl− and are soluble in water, meaning they provide evidence of past aqueous processes, which helps to constrain the type of environment at a particular region. On Earth, two main processes form chlorides: efflorescence and precipitation. Whereas on Earth these minerals are formed in more alkaline environments, the minerals on Mars form from more acidic fluids and the processes are connected to basaltic weathering. The key similarity between the formation of chlorides on the two planets is the presence of water. This is important because water is essential to life on Earth, and therefore drives the search for evidence of life on other planets. Chlorides are of particular interest because of their potential to preserve a biological signature through chemical sedimentation. In addition, their presence throughout the entire southern hemisphere of Mars suggests their formation have been an important process to the early history of Mars.
Methods for identification
The chloride salts were identified using THEMIS on board the 2001 Mars Odyssey orbiter. The spectrum acquired from THEMIS shows a featureless slope from wavenumber (~672 to 1475 cm−1). Few things describe this spectrally distinct feature, and thus has been concluded to be the result of chloride-bearing deposits. One such supporting terrestrial example is the identification of halite in Death Valley by instruments in the same wavelength as THEMIS. Further investigation of these deposits using the High Resolution Imaging Science Experiment (HiRISE) on the Mars Reconnaissance Orbiter (MRO) showed the features to be light-toned and irregularly-shaped fractures overlying small, degraded craters. Spectra from the Compact Reconnaissance Imaging Spectrometer (CRISM) on MRO was also used for comparison in lab experiments to explain the featureless slope observed in the THEMIS data. Known minerals on Earth were tested to see if they reproduced the same distinct THEMIS spectra. Pyrite was determined to not be a possible match for the mineral deposits on Mars. Flood basalt mixtures containing halite reproduced the spectra in some instances, reinforcing the conclusion that this THEMIS spectra, and thus the deposits, are chloride. However, the most definitive evidence that these are in fact chloride deposits will come from in situ observations on the Martian surface.
Terra Sirenum is a region in the southern highlands of Mars (approximately at 38.8°S, 221°E), with a distinguishing feature of a higher brightness as compared to the typical background soils. It is of particular interest because it is the location of the largest regional occurrence of chlorides. One study has interpreted six regions of chloride deposits (10 – 50 km2) in the lowest topographical levels of an inter-crater basin (300 – 400 km) as individual salt flats. Connecting channels between the salt flats provides evidence for a common origin, such as evaporation of water. Comparing these salt flats to ones observed on Earth, such as those in the Atacama Desert further supports the hypothesis of a formation due to evaporation. Using CRISM data, this study also observed phyllosilicates in the rims of craters and the surrounding ejecta to occur near the chlorides. Another study also observed phyllosilicates to be closely located to chlorides with CRISM, as well as THEMIS. Phyllosilicates also provide evidence for aqueous processes occurring during the Noachian period. Both studies determined that the phyllosilicates were deposited first.
- Osterloo, M. M. et al. (2010). "Geologic context of proposed chloride-bearing materials on Mars". Journal of Geophysical Research 115. Bibcode:2010JGRE..11510012O. doi:10.1029/2010JE003613.
- Goodall, Timothy M. et al. (2000). "Surface and subsurface sedimentary structures produced by salt crusts". Sedimentology 47 (1): 99–118. doi:10.1046/j.1365-3091.2000.00279.x.
- Osterloo, M. M. et al. (2008). "Chloride-Bearing Materials in the Southern Highlands of Mars". Science 319 (5870): 1651–1654. Bibcode:2008Sci...319.1651O. doi:10.1126/science.1150690. PMID 18356522.
- Jensen, H.B.; Glotch, T.D. (2011). "Investigation of the near-infrared spectral character of putative Martian chloride deposits". Journal of Geophysical Research 116. Bibcode:2011JGRE..116.0J03J. doi:10.1029/2011JE003887.
- Glotch, T. D. et al. (2010). "Distribution and formation of chlorides and phyllosilicates in Terra Sirenum, Mars". Geophysical Research Letters 37. Bibcode:2010GeoRL..3716202G. doi:10.1029/2010GL044557.
- Davila, Alfonso et al. (2011). "A large sedimnetary basin in the Terra Sirenum region of the southern highlands". Icarus 212: 579–589. Bibcode:2011Icar..212..579D. doi:10.1016/j.icarus.2010.12.023.
- Murchie, Scott L. et al. (2009). "A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter". Journal of Geophysical Research 114. Bibcode:2009JGRE..114.0D06M. doi:10.1029/2009JE003342.
- Pueyo, Juan Jose et al. (2001). "Neogene evaporites in desert volcanic environments: Atacama Desert, northern Chile". Sedimentology 48: 1411–1431. Bibcode:2002Sedim..48.1411P. doi:10.1046/j.1365-3091.2001.00428.x.
- Bibring, Jean-Pierre et al. (2006). "Global Mineralogical and Aqueous Mars History Derived from OMEGA/Mars Express Data". Science 312 (5772): 400–404. Bibcode:2006Sci...312..400B. doi:10.1126/science.1122659. PMID 16627738.