^1,2F. Javier Martín-Torres et al. (>10)*
¹Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), 18100 Armilla, Granada, Spain
²Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology, S98192 Kiruna, Sweden
*Find the extensive, full author and affiliation list on the publishers website

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Reference
Martín-Torres FJ et al. (2015) Transient liquid water and water activity at Gale crater on Mars. Nature Geoscience (in Press)
Link to Article [doi:10.1038/ngeo2412]

^1,2Richard G. Kraus, ³Seth Root, ⁴Raymond W. Lemke, ^1,5Sarah T. Stewart, ¹Stein B. Jacobsen, ⁴Thomas R. Mattsson

¹Department of Earth and Planetary Sciences, Harvard University, 20 Oxford Street, Cambridge, Massachusetts 02138, USA
²Shock Physics Group, Lawrence Livermore National Laboratory, PO Box 808, L-487, Livermore, California 94551-0808, USA
³Dynamic Material Properties Group, Sandia National Laboratory, PO Box 5800, Albuquerque, New Mexico 87185-1195, USA
⁴High Energy Density Physics Theory, Sandia National Laboratory, PO Box 5800, Albuquerque, New Mexico 87185-1189, USA
⁵Department of Earth and Planetary Sciences, UC Davis, One Shields Avenue, Davis, California 95616, USA

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Reference
Kraus RG, Root S, Lemke RW, Stewart ST, Jacobsen SB, Mattsson TR (2015) Impact vaporization of planetesimal cores in the late stages of planet Formation. Nature Geoscience 8, 269–272
Link to Article [doi:10.1038/ngeo2369]

¹Kimberly R. Kuhlman, ²Kumar Sridharan, ³Alexander Kvit
¹Planetary Science Institute, 1700 East Fort Lowell Blvd., Suite 106, Tucson, AZ 85719
²University of Wisconsin – Madison, Department of Engineering Physics, 1500 Engineering Drive, Madison, WI 53706
³University of Wisconsin – Madison, Materials Science Center & Department of Materials Science and Engineering, 1509 University Ave., Madison, WI 53706

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Reference
Kuhlman KR, Sridharan K, Kvit A (2015) Simulation of solar wind space weathering in orthopyroxene. Planetary and Space Science (in Press)
Link to Article [doi:10.1016/j.pss.2015.04.003]

¹Amira Elsenousy, ²Jennifer Hanley, ¹Vincent F. Chevrier
¹Arkansas Center for Space and Planetary Sciences, STON, University of Arkansas, 346 1/2 N. Arkansas Ave., Fayetteville, AR 72701, USA
²Southwest Research Institute, 1050 Walnut St, Suite 300, Boulder, CO 80302, USA

The WCL (Wet Chemistry Lab) instrument on board the Phoenix Lander identified the soluble ionic composition of the soil at the landing site. However, few studies have been conducted to understand the parent salts of these soluble ions. Here we studied the possible salt assemblages at the Phoenix landing site using two different thermodynamic models: FREZCHEM and Geochemist’s Workbench (GWB). Two precipitation pathways were used: evaporation (T<0Tusing only FREZCHEM). Through applying three different models of initial ionic concentrations (from sulfate to chlorate/perchlorate dominated), we calculated the resulting precipitated minerals. The results—through both freezing and evaporation—showed some common minerals that precipitated regardless of the ionic initial concentration. These ubiquitous minerals are magnesium chlorate hexahydrate Mg(ClO₃)₂⋅6H₂O, potassium perchlorate (KClO₄) and gypsum (CaSO₄⋅2H₂O). Other minerals evidence specific precipitation pathway. Precipitation of highly hydrated salts such as meridianiite (MgSO₄⋅11H₂O) and MgCl₂⋅12H₂O indicate freezing pathway, while precipitation of the low hydrated salts (anhydrite, kieserite and epsomite) indicate evaporation. The present hydration states of the precipitated hydrated minerals probably reflect the ongoing thermal processing and recent seasonally varying humidity conditions at the landing site, but these hydration states might not reflect the original depositional conditions. The simulations also showed the absence of Ca-perchlorate in all models, mainly because of the formation of two main salts: KClO₄ and gypsum which are major sinks for ClO⁻₄ and Ca²⁺ respectively. Finally, in consideration to the Martian life, it might survive at the very low temperatures and low water activities of the liquids formed. However, besides the big and widely recognized challenges to life posed by those extreme environmental parameters (especially low water activity), another main challenge for any form of life in such an environment is to maintain contact with the small droplets of the stable liquids in the regolith and to interact with life in other isolated droplets.

Reference
Elsenousy A, Hanley J, Chevrier VF (2015) Effect of evaporation and freezing on the salt paragenesis and habitability of brines at the Phoenix landing site. Earth and Planetary Science Letters 421, 39–46
Link to Article [doi:10.1016/j.epsl.2015.03.047]

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