Thermal expansion and lattice distortion of clathrate hydrates of cubic structures I and II

Belosludov, V. R.; Inerbaev, Talgat M.; Субботин, О. С.; Belosludov, Rodion V.; Kudoh, J.

doi:10.1016/s1472-7862(03)00072-8

Cited by 32 publications

(41 citation statements)

References 24 publications

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“…Gas molecules are caged in the clathrates. Researchers have found three kinds of hydrate structures: structure type-I, structure type-II and structure type-H (Belosludov et al, 2002;Ohgaki, Sugahara, & Suzuki, 2000;Purwanto et al, 2001). In our previous study (Zhan, 2005), structure type-I A US patent was issued for the use of Ar in the preservation of cut and segmented fresh fruits (Powrie et al, 1990).…”

Section: Introductionmentioning

confidence: 94%

Extending the shelf-life of asparagus spears with a compressed mix of argon and xenon gases

Zhang

Zhan

Wang

et al. 2008

LWT - Food Science and Technology

102

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Section: Introductionmentioning

confidence: 94%

Extending the shelf-life of asparagus spears with a compressed mix of argon and xenon gases

Zhang

Zhan

Wang

et al. 2008

LWT - Food Science and Technology

102

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“…Moreover, it has been shown that the size of the clathrate cages depends on their formation temperature. [35][36][37] This also leads us to investigate the influence of the size of cages on the resulting composition of clathrates formed in the low pressure and temperature conditions of the nebula.…”

Section: Introductionmentioning

confidence: 99%

Volatile inventories in clathrate hydrates formed in the primordial nebula

et al. 2010

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Examination of ambient thermodynamic conditions suggest that clathrate hydrates could exist in the martian permafrost, on the surface and in the interior of Titan, as well as in other icy satellites. Clathrate hydrates probably formed in a significant fraction of planetesimals in the solar system. Thus, these crystalline solids may have been accreted in comets, in the forming giant planets and in their surrounding satellite systems. In this work, we use a statistical thermodynamic model to investigate the composition of clathrate hydrates that may have formed in the primordial nebula. In our approach, we consider the formation sequence of the different ices occurring during the cooling of the nebula, a reasonable idealization of the process by which volatiles are trapped in planetesimals. We then determine the fractional occupancies of guests in each clathrate hydrate formed at given temperature. The major ingredient of our model is the description of the guest-clathrate hydrate interaction by a spherically averaged Kihara potential with a nominal set of parameters, most of which being fitted on experimental equilibrium data. Our model allows us to find that Kr, Ar and N 2 can be efficiently encaged in clathrate hydrates formed at temperatures higher than ∼ 48.5 K in the primitive nebula, instead of forming pure condensates below 30 K. However, we find at the same time that the determination of the relative abundances of guest species incorporated in these clathrate hydrates strongly depends on the choice of the parameters of the Kihara potential and also on the adopted size of cages. Indeed, testing different potential parameters, we have noted that even minor dispersions between the different existing sets can lead to non-negligible variations in the determination of the volatiles trapped in clathrate hydrates formed in the primordial nebula. However, these variations are not found to be strong enough to reverse the relative abundances between the different volatiles in the clathrate hydrates themselves. On the other hand, if contraction or expansion of the cages due to temperature variations are imposed in our model, the Ar and Kr mole fractions can be modified up to several orders of magnitude in clathrate hydrates. Moreover, mole fractions of other molecules such as N 2 or CO are also subject to strong changes with the variation of the size of the cages. Our results may affect the predictions of the composition of the planetesimals formed in the outer solar system. In particular, the volatile abundances calculated in the giant planets atmospheres should be altered because these quantities are proportional to the mass of accreted and vaporized icy planetesimals. For similar reasons, the estimates of the volatile budgets accreted by icy satellites and comets may also be altered by our calculations. For instance, under some conditions, our calculations predict that the abundance of argon in the atmosphere of Titan should be higher than the value measured by Huygens. Moreover, the Ar abundance in comets...

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“…36) It was show in 23,24) for methane hydrate the coincidence of the calculated results and experimental data is sufficiently good at temperatures below 200 K. At higher temperatures than 195 K the methane hydrate exists as a metastable phase, and the calculated relative changes of the volume V/V (195 K) The calculated temperature dependence of pressure in hydrate at heating ice from T ¼ 195 K at pressure P ¼ 0:1 MPa are displayed in Fig. 9.…”

Section: Hydrate Phases Immersed In the Ice Phasementioning

confidence: 69%

“…The lattice dynamic (LD) calculations also give larger values of thermal expansion of gas hydrates than that of the ice. [22][23][24] For practical application of clathrate hydrates as storage materials, it is important to know the region of stability of these compounds (there are several type of gas hydrate structures with different cage shapes) at various pressure and temperatures. Currently, analytical theories of clathrate compounds, which allow one to construct the T-P diagram of gas hydrates, are still based on the pioneering work of van der Waals and Platteeuw.…”

Section: Introductionmentioning

confidence: 99%

Physical and Chemical Properties of Gas Hydrates: Theoretical Aspects of Energy Storage Application

et al. 2007

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A model has been developed permitting to accurately predict on molecular level phase diagram of the clathrate hydrates. This model allows to take into account the influence of guest molecules on the host lattice and to extend the interval of temperatures and pressures of computed thermodynamic potentials and significantly improves known van der Waals and Platteeu theory. The theoretical study of phase equilibrium in gas-gas hydrate-ice Ih system for methane and xenon hydrates has been performed. The obtained results are in a good agreement with experimental data. A new interpretation of so-called self-preservation effect has been proposed. The self-preservation of gas hydrates can be connected with differences in thermal expansions of ice Ih and gas hydrates. This is confirmed by calculations performed for methane and mixed methane-ethane hydrates.

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Thermal expansion and lattice distortion of clathrate hydrates of cubic structures I and II

Cited by 32 publications

References 24 publications

Extending the shelf-life of asparagus spears with a compressed mix of argon and xenon gases

Extending the shelf-life of asparagus spears with a compressed mix of argon and xenon gases

Volatile inventories in clathrate hydrates formed in the primordial nebula

Physical and Chemical Properties of Gas Hydrates: Theoretical Aspects of Energy Storage Application

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