Clathrate formation in water-noble gas (Hydrogen) systems at high pressures

Dyadin, Yu. A.; Larionov, Eduard G.; Aladko, E. Ya.; Manakov, Andrey Yu.; Zhurko, F. V.; Mikina, T. V.; Komarov, V. Yu.; Грачев, Е. В.

doi:10.1007/bf02903454

Cited by 142 publications

(108 citation statements)

References 12 publications

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“…Why then is only xenon depleted in terrestrial and martian atmospheres because argon also enhances the formation of clathrates up to 0.6 GPa at room temperature and up to 3.0 GPa at 140°C (14)? Previous studies of phase equilibria in rare gas-water systems under pressure (3,30) have led to the conclusion that the hydrate stability diminishes from xenon to neon. Argon can enter or leave the cavity relatively easily; the enthalpy change (when 1 mol of inert gas is sorbed within the clathrate cavity) is Ϫ2.82 kcal/mol whereas it is Ϫ5.37 kcal/mol for xenon (11), which is larger (4.56-Å diameter).…”

mentioning

confidence: 99%

High-pressure transformations in xenon hydrates

Sanloup

Mao

Hemley

2001

Proc. Natl. Acad. Sci. U.S.A.

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A high-pressure investigation of the Xe⅐H2O chemical system was conducted by using diamond-anvil cell techniques combined with in situ Raman spectroscopy, synchrotron x-ray diffraction, and laser heating. Structure I xenon clathrate was observed to be stable up to 1.8 GPa, at which pressure it transforms to a new Xe clathrate phase stable up to 2.5 GPa before breaking down to ice VII plus solid xenon. The bulk modulus and structure of both phases were determined: 9 ؎ 1 GPa for Xe clathrate A with structure I (cubic, a ‫؍‬ 11.595 ؎ 0.003 Å, V ‫؍‬ 1,558.9 ؎ 1.2 Å 3 at 1.1 GPa) and 45 ؎ 5 GPa for Xe clathrate B (tetragonal, a ‫؍‬ 8.320 ؎ 0.004 Å, c ‫؍‬ 10.287 ؎ 0.007 Å, V ‫؍‬ 712.1 ؎ 1.2 Å 3 at 2.2 GPa). The extended pressure stability field of Xe clathrate structure I (A) and the discovery of a second Xe clathrate (B) above 1.8 GPa have implications for xenon in terrestrial and planetary interiors.

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confidence: 99%

High-pressure transformations in xenon hydrates

Sanloup

Mao

Hemley

2001

Proc. Natl. Acad. Sci. U.S.A.

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“…1. Two principal thermal states of icy satellite interiors are distinguished, labeled Chizhov 1993 andGrasset 2007), and the dissociation curves of major clathrate hydrates under pressure (Sloan 1998, and references therein, Dyadin et al 1997a, 1997b, 1997c, Manakov et al 2001. For clathrate hydrates, solid-solid phase transitions under pressure are not specified to preserve legibility of the diagram.…”

Section: Phase Diagram Of H 2 O-rich Phases Under Pressurementioning

confidence: 99%

Subsurface Water Oceans on Icy Satellites: Chemical Composition and Exchange Processes

et al. 2010

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The state of knowledge about the structure and composition of icy satellite interiors has been significantly extended by combining direct measurements from spacecraft, laboratory experiments, and theoretical modeling. The existence of potentially habitable liquid water reservoirs on icy satellites is dependent on the radiogenic heating of the rock component, additional contributions such as the dissipation of tidal energy, the efficiency of heat transfer to the surface, and the presence of substances that deplete the freezing point of liquid water. This review summarizes the chemical evolution of subsurface liquid water oceans, taking into account a number of chemical processes occuring in aqueous environments and partly related to material exchange with the deep interior. Of interest are processes occuring at the transitions from the liquid water layer to the ice layers above and below, involving the possible formation of clathrate hydrates and high-pressure ices on large icy satellites. In contrast, water-rock exchange is important for the chemical evolution of the liquid water layer if the latter is in contact with ocean floor rock on small satellites. The composition of oceanic floor deposits depends on ambient physical conditions and ocean chemistry, and their evolutions through time. In turn, physical properties of the ocean floor affect the circulation of oceanic water and related thermal effects due to tidally-induced porous flow and aqueous alteration of ocean floor rock.

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“…Londono and co-workers proved this possibility by accommodating helium inside the cavities of ice II, giving the first helium hydrate [3]. Following that, it was also shown that neon could be accommodated inside ice II [4]. Later, Vos and co-workers reported the formation of hydrogen hydrate of ice II and ice I c structures at high pressure [5] whose stability is then explained using simulation and theoretical calculation [6,7]; from then, the possibility of neon to form a hydrate of ice I c structure was examined [8].…”

Section: Introductionmentioning

confidence: 95%

Inclusion of Neon Inside Ice I_cand Its Influence to the Ice Structure

et al. 2012

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A hybrid type of grand-canonical Monte Carlo simulation is carried out to investigate the accommodation of guest particle, i.e. neon, inside ice I c and its influence to the ice structure. The simulation is extended from low pressure and temperature where the pure ice I c structure is stable. As the compression proceeds, ice I c structure become unstable due to the high pressure, and then at higher pressure it is shown that a large amount of neon can be kept inside the ice giving a stable neon hydrate of ice I c structure with the neon-to-water molar ratio close to unity. The key factor in stabilizing ice structure by guest particle is clarified by carrying out simulation with different magnitudes of Lennard-Jones (LJ) parameter wg which mainly determine the depth of LJ potential well of interaction between guest and host particles.

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Clathrate formation in water-noble gas (Hydrogen) systems at high pressures

Cited by 142 publications

References 12 publications

High-pressure transformations in xenon hydrates

High-pressure transformations in xenon hydrates

Subsurface Water Oceans on Icy Satellites: Chemical Composition and Exchange Processes

Inclusion of Neon Inside Ice I_cand Its Influence to the Ice Structure

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Clathrate formation in water-noble gas (Hydrogen) systems at high pressures

Cited by 142 publications

References 12 publications

High-pressure transformations in xenon hydrates

High-pressure transformations in xenon hydrates

Subsurface Water Oceans on Icy Satellites: Chemical Composition and Exchange Processes

Inclusion of Neon Inside Ice Icand Its Influence to the Ice Structure

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Inclusion of Neon Inside Ice I_cand Its Influence to the Ice Structure