^1,2Yang, Y., ²Zhang, X., ³Liu, S.-A., ⁴Zhou, T., ⁴Fan, H., ²Yu, H., ^1,2Cheng, W., ²Huang, F.
Journal of Analytical Atomic Spectroscopy 33, 1777-1783 Link to Article [DOI: 10.1039/c8ja00249e]
¹State Key Laboratory of Soil and Sustainable Agriculture, Institute of Soil Science, Chinese Academy of Sciences, Nanjing, 210008, China
²School of Earth and Space Sciences, University of Science and Technology of China, Hefei, Anhui 230026, China
³State Key Laboratory of Geological Process and Mineral Resources, China University of Geosciences, Beijing, 100083, China
⁴State Key Laboratory of Ore Deposit Geochemistry, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang, Guizhou 550081, China

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¹Hontsova, S.S., ²Danilenko, I.A., ²Yakovlev, G.A., ²Petrova, E.V., ¹Maksimova, E.M., ¹Nauhatsky, I.A.
AIP Conference Proceedings 2015, 020029 Link to Article [DOI: 10.1063/1.5055102]
¹Department of Theoretical Physics and Solid State, Institute of Physical – Technical, Crimean Federal University, Simferopol, 295007, Russian Federation
²Department of Physical Techniques and Devices for Quality Control, Institute of Physics and Technology, Ural Federal University, Ekaterinburg, 620002, Russian Federation

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^1,2Emmal Safi, ²Stephen P.Thompson, ¹Aneurin Evans, ²Sarah J.Day, ²Claire A.Murray, ²Annabelle R.Baker, ¹Joana M.Oliveira, ¹Jacco Th.van Loon
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2018.10.034]
¹Astrophysics Group, Lennard-Jones Laboratories, Keele University, Keele, Staffordshire, ST5 5BG, UK
²Diamond Light Source, Harwell Science and Innovation Campus, Didcot, Oxfordshire, OX11 0DE, UK
Copyright Elsevier

Water on the present day Martian surface is thought to exist in two thermally distinct sub-surface reservoirs: as ice in the cryosphere and as groundwater located deeper in the crust. These sub-surface environments are thought to contain saline, rather than pure, water and laboratory studies on whether or not clathrate hydrates can form in such environments are lacking. We fill this gap by performing synchrotron radiation X-ray powder diffraction to investigate the formation and evolution of clathrate hydrates in weak chloride solutions at CO₂ pressures, and over temperature ranges, that are similar to those found in the Martian regolith. We have found that clathrate hydrates can form under conditions relevant to the Martian cryosphere, despite the presence of chloride salts. We find that the dissociation temperatures for CO₂ clathrate hydrates formed in saline solutions are depressed by 10–20 K relative to those formed in pure water, depending on the nature of the salt and the CO₂ pressure. We suggest that the inhibiting effect that salts such as MgCl₂, CaCl₂ and NaCl have on clathrate hydrate formation could also be related to the salts’ effect on the formation of the low temperature phase of ice. However, despite the inhibiting effect of the salts, we conclude that the presence of clathrate hydrates should still be possible under conditions likely to exist within the Martian cryosphere.