Saturday, 28 March 2015

Hydrated silicate minerals in the Mariner Valley, Mars.

Hydrated minerals (minerals containing water) are considered to be evidence of the former presence of liquid water on Mars. They have been observed at a number of locations on the planet, and seem to have been formed in a number of phases, with the oldest, Noachian, deposits (thought to be approximately 4100 to 3700 million years ago) frequently containing hydrated phyllosilicates, younger, Hesperian deposits (from about 2700 million years ago to between 3200 and 2000 million years ago) containing hydrated sulphates and the youngest, Amazonian, deposits (anything younger than Hesperian) containing hydrated ferric oxides. A variety of hydrated minerals have previously been detected in the Valles Marineris (Mariner Valley), the largest canyon system on Mars, where the central portion contains extensive hydrated sulphate deposits, and hydrated clays, silicates and iron minerals have also been observed.

In a paper published in the journal Geophysical Research Letters on 30 December 2014, Catherine Weitz of the Planetary Science Institute, Janice Bishop of the SETI Institute, Leslie Baker of the Department of Geological Sciences at the University of Idaho and Daniel Berman, also of the Planetary Science Institute describe the discovery of iron rich allophane or opal deposits (hydrated silicates) in the Coprates Chasma region of the central Valles Marineris.

(Top) Mars Orbiter Laser Altimeter topography overlain on Thermal Emission Imaging System (THEMIS) daytime infrared mosaic of central Valles Marineris, including Melas, Coprates, and Eos chasmata. The yellow rectangle indicates the location of the bottom left figure. (Bottom left) Portion of HRSC image H0438_0000_ND4 showing Coprates Chasma. The yellow rectangle identifies the location of study region and bottom right figure. (Bottom Right) Portion of CTX image P18_008141_1647 with CRISM spectral parameters derived from image HRL0000A8F6 overlain in colour (red is olivine index, green is band depth at 1.9 μm, and blue is doublet between 2.2 and 2.3 μm). The Fe-rich allophane/opal deposits are outlined in yellow, whereas blue lines outline smectite exposures. Weitz et al. (2014).

Allophane and opal are semi-amorphous hydrated aluminium silicates, which generally form as weathering products of volcanic rocks on Earth. They are considered to be quite unstable, particularly in their high-iron forms, which tend to break down into iron rich clays. While chemical weathering processes on Mars are thought to be slower than on Earth, it is still unlikely that these minerals could have persisted at the surface for very long periods of time, suggesting that they have either been formed recently (in geological terms) by the action of water, or have been recently exposed by active geological movements, either of which would be a significant discovery.

Expanded views of the areas outlined by black boxes in the bottom right image above. (b and c) Hydrated nanophase Fe-rich allophane/opal corresponds to materials within yellow outlines. Portion of HiRISE images ESP_033010_1645 and PSP_008141_1645. (d) Channel containing Fe-rich allophane/opal (red arrows). Portion of HiRISE image PSP_008141_1645. (e) Example of smectites along the wall rock. Weitz et al. (2014).

The Coprates Chasma region is interpreted as a graben structure, which is to say an area where rock movements have drawn two areas of planetary crust apart, resulting in thinning of the crust in the central area, which in turn tends to lead to subsidence and slumping. The allophane/opal deposits are exposed on an area of slumping (landslips) thought to be in the region of 50-100 million years old. It is unclear if these minerals predated this slumping, and have been exposed by it, thereby potentially representing a greater reserve buried beneath the surface, or whether they are younger material that has formed at the surface as the result of the weathering of other minerals exposed by the slumping.

HiRISE DTMperspective view at 2X vertical exaggeration with CRISM spectral parameters overlain in colour (red is olivine index, green is band depth at 1.9 μm, and blue is doublet between 2.2 and 2.3 μm). The red arrows identify the eastern Fe-rich allophane/opal deposit (whitish blue), which extends across 940m in elevation, whereas the green arrows identify exposures of smectites within the wall rock (yellow-light green). HiRISE stereo pair images PSP_008141_1645 and PSP_007785_1645 were used to make the DTM. Weitz et al. (2014).

See also…

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