Multiple mineral horizons in layered outcrops at Mawrth Vallis, Mars, signify changing geochemical environments on early Mars

1,2Janice L.Bishop,2Christoph Gross,1,3 Jacob Danielsen,4Mario Parente,5Scott L.Murchie,6 Briony Horgan,7James J.Wray,6Christina Viviano,6Frank P.Seelos
Icarus (in Press) Link to Article []
1SETI Institute, Mountain View, CA, United States of America
2Freie Universität Berlin, Berlin, Germany
3San Jose State University, San Jose, CA, United States of America
4University of Massachusetts at Amherst, Amherst, MA, United States of America
5Johns Hopkins University Applied Physics Lab, Laurel, MD, United States of America
6Purdue University, West Lafayette, IN, United States of America
7Georgia Institute of Technology, Atlanta, GA, United States of America
Copyright Elsevier

Refined calibrations of CRISM images are enabling identification of smaller deposits of unique aqueous materials on Mars that reveal changing environmental conditions at the region surrounding Mawrth Vallis. Through characterization of these clay-sulfate assemblages and their association with the layered, phyllosilicate units of this region, more details of the aqueous geochemical history can be gleaned. A stratigraphy including five distinct mineral horizons is mapped using compositional data from CRISM over CTX and HRSC imagery across 100s of km and from CRISM over HiRISE imagery across 100s of meters. Transitions in mineralogic units were characterized using visible/near-infrared (VNIR) spectral properties and surface morphology. We identified and characterized complex “doublet” type spectral signatures with two bands between 2.2 and 2.3 μm at one stratigraphic horizon. Based on comparisons with terrestrial sites, the spectral “doublet” unit described here may reflect the remnants of a salty, evaporative period that existed on Mars during the transition from formation of Fe-rich phyllosilicates to Al-rich phyllosilicates. Layered outcrops observed at Mawrth Vallis are thicker than in other altered regions of Mars, but may represent processes that were more widespread in wet regions of the planet during its early history. The aqueous geochemical environments supporting the outcrops observed here include: (i) the formation of Fe3+-rich smectites in a warm and wet environment, (ii) overlain by a thin ferrous-bearing clay unit that could be associated with heating or reducing conditions, (iii) followed by a transition to salty and/or acidic alteration phases and sulfates (characterized by the spectral “doublet” shape) in an evaporative setting, (iv) formation of Al-rich phyllosilicates through pedogenesis or acid leaching, and (v) finally persistence of poorly crystalline aluminosilicates marking the end of the warm climate on early Mars. The “doublet” type units described here are likely composed of clay-sulfate assemblages formed in saline, acidic evaporative environments similar to those found in Western Australia and the Atacama desert. Despite the chemically extreme and variable waters present at these terrestrial, saline lake environments, active ecosystems are present; thus, these “doublet” type units may mark exciting areas for continued exploration important to astrobiology on Mars.


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