Physical Properties of Gas Hydrates: A Review

Gabitto, Jorge; Tsouris, Costas

doi:10.1155/2010/271291

Cited by 139 publications

(84 citation statements)

References 58 publications

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“…Clathrates can exist mainly under two types of structure called structure I (SI) and structure II (SII) that contain two types of cavities (small and large) whose number, size, and hydrate number n hyd (mean number of water molecule per molecule of trapped species) differ and depend on the size of the trapped molecules (see Sloan & Koh 2008;Gabitto & Tsouris 2010, for a review). The hydrate number n hyd therefore provides the average number of H 2 O molecules needed to form cages around each gas species x trapped,…”

Section: Thermodynamics Parameters Of Condensation and Clathrate Formmentioning

confidence: 99%

“…Four of these five molecules (CO, CH 4 , CO 2 , H 2 S) form individually a SI structure of clathrate (Davidson et al 1987;Dartois 2011;Handa 1986b;Anderson 2003;Miller 1961) and N 2 is the only one molecule forming a SII-structure (Chazallon & Kuhs 2002;Sloan & Koh 2008), leading to small differences in n hyd . All volatile molecules studied in this work are small enough to enter both the small and large cavities (Sloan & Koh 2008;Gabitto & Tsouris 2010). The ideal hydrate number n hyd in the case of a maximum occupancy of the cages (all cages are filled) is equal to 5.75 (resp.…”

Section: Thermodynamics Parameters Of Condensation and Clathrate Formmentioning

confidence: 99%

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From stellar nebula to planetesimals

Marboeuf

Thiabaud

Alibert

et al. 2014

A&A

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Context. Solar and extrasolar comets and extrasolar planets are the subject of numerous studies in order to determine their chemical composition and internal structure. In the case of planetesimals, their compositions are important as they govern in part the composition of future planets. Aims. The present works aims at determining the chemical composition of icy planetesimals, believed to be similar to present day comets, formed in stellar systems of solar chemical composition. The main objective of this work is to provide valuable theoretical data on chemical composition for models of planetesimals and comets, and models of planet formation and evolution. Methods. We have developed a model that calculates the composition of ices formed during the cooling of the stellar nebula. Coupled with a model of refractory element formation, it allows us to determine the chemical composition and mass ratio of ices to rocks in icy planetesimals throughout in the protoplanetary disc. Results. We provide relationships for ice line positions (for different volatile species) in the disc, and chemical compositions and mass ratios of ice relative to rock for icy planetesimals in stellar systems of solar chemical composition. From an initial homogeneous composition of the nebula, a wide variety of chemical compositions of planetesimals were produced as a function of the mass of the disc and distance to the star. Ices incorporated in planetesimals are mainly composed of H 2 O, CO, CO 2 , CH 3 OH, and NH 3 . The ice/rock mass ratio is equal to 1 ± 0.5 in icy planetesimals following assumptions. This last value is in good agreement with observations of solar system comets, but remains lower than usual assumptions made in planet formation models, taking this ratio to be of 2-3.

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Section: Thermodynamics Parameters Of Condensation and Clathrate Formmentioning

confidence: 99%

Section: Thermodynamics Parameters Of Condensation and Clathrate Formmentioning

confidence: 99%

From stellar nebula to planetesimals

Marboeuf

Thiabaud

Alibert

et al. 2014

A&A

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“…Water molecules form frameworks of large cavities as a result of the hydrogen bond within the water molecule which enclose the guest gas molecule. The gas hydrate is thermodynamicaly stable because of the interaction between the water and the gas molecules [4]. Gases hydrates samples have been discovered from many places-19 or more areas worldwide and are believed to be deposited at roughly 77 areas including the Antarctica and Siberia.…”

Section: Nature Of Gas Hydrate Depositsmentioning

confidence: 99%

“…Larger molecules with diameters: 7 Å < d < 9 Å, i.e. iso-pentane and 2, 2-dimethylbutane form sH gas hydrates in the presence of smaller molecules like methane or nitrogen [4] as shown in Table 2. Flow assurance problems caused by gas hydrates occur as a result of slow cooling of oil and gas in pipeline or rapid cooling due to depressurizing across the valves installed with the pipeline or distribution systems.…”

Section: Properties Of Gas Hydratesmentioning

confidence: 99%

“…There are also secondary influencing factors which favor hydrate formation such as high fluid velocities, agitation, pressure, pulsations or any source of fluid turbulence, the presence of CO 2 and H 2 S [4]. Understanding the properties of gas hydrates is crucial to the exploration and production of these enormous deposits of methane gas.…”

Section: Properties Of Gas Hydratesmentioning

confidence: 99%

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Gas Hydrate—Properties, Formation and Benefits

Aregbe¹

2017

OJOGas

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There are numerous gas hydrate reserves all over the world, especially in permafrost regions and ocean environments. The abundance of gas hydrate reserves is estimated to be more than twice of the combined carbon of coal, conventional gas and petroleum reserves. These hydrate deposits hold significant amount of energy which can make hydrate a sustainable energy resource. The comprehensive research on the properties and formation of methane hydrates is paramount to ensure efficient and effective exploration and development of hydrate reserves. Natural gas is mostly distributed for different purposes through pipelines or pressure vessels such as dry gas, compressed gas or liquefied gas, which means transporting natural gas creates serious safety concerns because methane is highly flammable and almost impossible to detect any leak without using odorant. Alternatively, natural gas can be stored and transported as gas hydrate turns solid or slurry. Gas hydrate can be stored at equilibrium conditions with either saturation temperature or pressure. The equilibrium conditions are influenced by the cost and weight of storage vessel. Hydrate can be transported either as slurry or solid depending on the location of target or destination. The slurry form is usually a better option for distance of approximately 2500 mile or less while the solid form can be used for distances of roughly 3500 miles or more. The paper examines the properties, formation and benefits of gas hydrate. The suitability of gas hydrate as a sustainable energy resource and the possibility of using gas hydrate for the transportation and storage of natural gas (methane) are also stated. Natural gas transportation and storage as gas hydrate will create effectively and efficiently alternative bulk gas transportation and storage for future use of the gas.

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Imaging methane hydrates growth dynamics in porous media using synchrotron X‐ray computed microtomography

Kerkar

Horvat

Jones

et al. 2014

Geochem Geophys Geosyst

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Commercial-scale methane (CH 4 ) extraction from natural hydrate deposits remains a challenge due to, among other factors, a poor understanding of hydrate-host sediment interactions under low-temperature and high-pressure conditions that are conducive to their existence. We report the use of synchrotron X-ray computed microtomography (CMT) to image, for the first time, time-resolved pore-scale methane CH 4 hydrate growth from an aqueous solution containing 5 wt % barium chloride (BaCl 2 ) and pressurized CH 4 hosted in glass beads, all contained in an aluminum cell with an effective volume of 3.5 mL. Multiple two-dimensional (2-D) cross-sectional images show CH 4 hydrates, with 7.5 mm resolution, distributed in patches throughout the system without dependence on distance from the cell walls. The time-resolved three-dimensional (3-D) images, constructed from the 2-D slices, exhibited pore-filling hydrate formation from dissolved CH 4 gas, similar to natural CH 4 hydrates (sI) in the marine environment. Furthermore, the 3-D images show that the aqueous phase was the wetting phase of the glass beads, i.e., the host and the formed hydrate were separated by an aqueous layer. These results provide some fundamental understanding of the nucleation phenomenon of gas hydrate formation at the pore scale. Pore-filling CH 4 hydrate growth is likely to result in a reduced bulk modulus, and thus, could affect seafloor stability during the reverse phenomenon, i.e., dissociation of natural hydrate deposits.

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Physical Properties of Gas Hydrates: A Review

Cited by 139 publications

References 58 publications

From stellar nebula to planetesimals

From stellar nebula to planetesimals

Gas Hydrate—Properties, Formation and Benefits

Imaging methane hydrates growth dynamics in porous media using synchrotron X‐ray computed microtomography

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