Carbon dioxide clathrate

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Carbon dioxide hydrate or carbon dioxide clathrate is a snow-like crystalline substance composed of water ice and carbon dioxide. [1] It normally is a Type I gas clathrate. [2] There has also been some experimental evidence for the development of a metastable Type II phase at a temperature near the ice melting point. [3] [4] [5] The clathrate can exist below 283K (10 °C) at a range of pressures of carbon dioxide. CO2 hydrates are widely studied around the world due to their promising prospects of carbon dioxide capture from flue gas and fuel gas streams relevant to post-combustion and pre-combustion capture. [6] [7] [8] [9] It is also quite likely to be important on Mars due to the presence of carbon dioxide and ice at low temperatures.

Contents

History

The first evidence for the existence of CO2 hydrates dates back to the year 1882, when Zygmunt Florenty Wróblewski [10] [11] [12] reported clathrate formation while studying carbonic acid. He noted that gas hydrate was a white material resembling snow and could be formed by raising the pressure above a certain limit in his H2O - CO2 system. He was the first to estimate the CO2 hydrate composition, finding it to be approximately CO2•8H2O. He also mentions that "...the hydrate is only formed either on the walls of the tube, where the water layer is extremely thin or on the free water surface... (from French)" This already indicates the importance of the surface available for reaction (i.e. the larger the surface the better). Later on, in 1894, M. P. Villard deduced the hydrate composition as CO2•6H2O. [13] Three years later, he published the hydrate dissociation curve in the range 267 K to 283 K (-6 to 10 °C). [14] Tamman & Krige measured the hydrate decomposition curve from 253 K down to 230 K in 1925 [15] and Frost & Deaton (1946) determined the dissociation pressure between 273 and 283 K (0 and 10 °C). [16] Takenouchi & Kennedy (1965) measured the decomposition curve from 45 bars up to 2 kbar (4.5 to 200 MPa). [17] The CO2 hydrate was classified as a Type I clathrate for the first time by von Stackelberg & Muller (1954). [18]

Importance

Earth

In this mosaic taken by the Mars Global Surveyor: Aram Chaos - top left and Iani Chaos - bottom right. A river-bed-like outflow channel can be seen, originating from Iani Chaos and extending towards the top of the image. Aram Chaos.jpg
In this mosaic taken by the Mars Global Surveyor: Aram Chaos - top left and Iani Chaos - bottom right. A river-bed-like outflow channel can be seen, originating from Iani Chaos and extending towards the top of the image.

On Earth, CO2 hydrate is mostly of academic interest. Tim Collett of the United States Geological Survey (USGS) proposed pumping carbon dioxide into subsurface methane clathrates, thereby releasing the methane and storing the carbon dioxide. [19] As of 2009, ConocoPhillips is working on a trial on the Alaska North Slope with the US Department of Energy to release methane in this way. [20] [19] At first glance, it seems that the thermodynamic conditions there favor the existence of hydrates, yet given that the pressure is created by sea water rather than by CO2, the hydrate will decompose. [21] Recently, Professor Praveen Linga and his group in collaboration with ExxonMobil have demonstrated the first-ever experimental evidence of the stability of carbon dioxide hydrate in deep-oceanic sediments. [22] [23] [24]

Mars

However, it is believed that CO2 clathrate might be of significant importance for planetology. CO2 is an abundant volatile on Mars. It dominates in the atmosphere and covers its polar ice caps much of the time. In the early seventies, the possible existence of CO2 hydrates on Mars was proposed. [25] Recent consideration of the temperature and pressure of the regolith and of the thermally insulating properties of dry ice and CO2 clathrate [26] suggested that dry ice, CO2 clathrate, liquid CO2, and carbonated groundwater are common phases, even at Martian temperatures. [27] [28] [29]

If CO2 hydrates are present in the Martian polar caps, as some authors suggest, [30] [31] [32] [28] then the polar cap can potentially melt at depth. Melting of the polar cap would not be possible if it was composed entirely of pure water ice (Mellon et al. 1996). This is because of the clathrate's lower thermal conductivity, higher stability under pressure, and higher strength, [33] as compared to pure water ice.

The question of a possible diurnal and annual CO2 hydrate cycle on Mars remains, since the large temperature amplitudes observed there cause exiting and reentering the clathrate stability field on a daily and seasonal basis. The question is, then, can gas hydrate being deposited on the surface be detected by any means? The OMEGA spectrometer on board Mars Express returned some data, which were used by the OMEGA team to produce CO2 and H2O-based images of the South polar cap. No definitive answer has been rendered with respect to Martian CO2 clathrate formation.[ citation needed ]

The decomposition of CO2 hydrate is believed to play a significant role in the terraforming processes on Mars, and many of the observed surface features are partly attributed to it. For instance, Musselwhite et al. (2001) argued that the Martian gullies had been formed not by liquid water but by liquid CO2, since the present Martian climate does not allow liquid water existence on the surface in general. [34] This is especially true in the southern hemisphere, where most of the gully structures occur. However, water can be present there as ice Ih, CO2 hydrates or hydrates of other gases. [35] [36] All these can be melted under certain conditions and result in gully formation. There might also be liquid water at depths >2 km under the surface (see geotherms in the phase diagram). It is believed that the melting of ground-ice by high heat fluxes formed the Martian chaotic terrains. [37] Milton (1974) suggested the decomposition of CO2 clathrate caused rapid water outflows and formation of chaotic terrains. [38] Cabrol et al. (1998) proposed that the physical environment and the morphology of the south polar domes on Mars suggest possible cryovolcanism. [39] The surveyed region consisted of 1.5 km-thick-layered deposits covered seasonally by CO2 frost [40] underlain by H2O ice and CO2 hydrate at depths > 10 m. [25] When the pressure and the temperature are raised above the stability limit, clathrate is decomposed into ice and gases, resulting in explosive eruptions.

Still a lot more examples of the possible importance of the CO2 hydrate on Mars can be given. One thing remains unclear: is it really possible to form hydrate there? Kieffer (2000) suggests no significant amount of clathrates could exist near the surface of Mars. [41] Stewart & Nimmo (2002) find it is extremely unlikely that CO2 clathrate is present in the Martian regolith in quantities that would affect surface modification processes. [42] They argue that long term storage of CO2 hydrate in the crust, hypothetically formed in an ancient warmer climate, is limited by the removal rates in the present climate. [42] Baker et al. 1991 suggests that, if not today, at least in the early Martian geologic history the clathrates may have played an important role for the climate changes there. [43] Since not too much is known about the CO2 hydrates formation and decomposition kinetics, or their physical and structural properties, it becomes clear that all the above-mentioned speculations rest on extremely unstable bases.

Moons

On Enceladus decomposition of carbon dioxide clathrate is a possible way to explain the formation of gas plumes. [44]

In Europa (moon), clathrate should be important for storing carbon dioxide. In the conditions of the subsurface ocean in Europa, carbon dioxide clathrate should sink, and therefore not be apparent at the surface. [44]

Phase diagram

CO2 hydrate phase diagram. The black squares show experimental data. The lines of the CO2 phase boundaries are calculated according to the Intern. thermodyn. tables (1976). The H2O phase boundaries are only guides to the eye. The abbreviations are as follows: L - liquid, V - vapor, S - solid, I - water ice, H - hydrate. CO2HydrPhaseDiagram.jpg
CO2 hydrate phase diagram. The black squares show experimental data. The lines of the CO2 phase boundaries are calculated according to the Intern. thermodyn. tables (1976). The H2O phase boundaries are only guides to the eye. The abbreviations are as follows: L - liquid, V - vapor, S - solid, I - water ice, H - hydrate.

The hydrate structures are stable at different pressure-temperature conditions depending on the guest molecule. Here is given one Mars-related phase diagram of CO2 hydrate, combined with those of pure CO2 and water. [46] CO2 hydrate has two quadruple points: (I-Lw-H-V) (T = 273.1 K; p = 12.56 bar or 1.256 MPa) and (Lw-H-V-LHC) (T = 283.0 K; p = 44.99 bar or 4.499 MPa). [47] CO2 itself has a triple point at T = 216.58 K and p = 5.185 bar (518.5 kPa) and a critical point at T = 304.2 K and p = 73.858 bar (7.3858 MPa). The dark gray region (V-I-H) represents the conditions at which CO2 hydrate is stable together with gaseous CO2 and water ice (below 273.15 K). On the horizontal axes the temperature is given in kelvins and degrees Celsius (bottom and top respectively). On the vertical ones are given the pressure (left) and the estimated depth in the Martian regolith (right). The horizontal dashed line at zero depth represents the average Martian surface conditions. The two bent dashed lines show two theoretical Martian geotherms after Stewart & Nimmo (2002) at 30° and 70° latitude. [42]

Related Research Articles

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<span class="mw-page-title-main">Clathrate hydrate</span> Crystalline solid containing molecules caged in a lattice of frozen water

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<span class="mw-page-title-main">Dry ice</span> Solid carbon dioxide

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<span class="mw-page-title-main">Terraforming of Mars</span> Hypothetical modification of Mars into a habitable planet

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<span class="mw-page-title-main">Mare Australe quadrangle</span> Map of Mars

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<span class="mw-page-title-main">Water on Mars</span> Study of past and present water on Mars

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<span class="mw-page-title-main">Martian polar ice caps</span> Polar water ice deposits on Mars

The planet Mars has two permanent polar ice caps. During a pole's winter, it lies in continuous darkness, chilling the surface and causing the deposition of 25–30% of the atmosphere into slabs of CO2 ice (dry ice). When the poles are again exposed to sunlight, the frozen CO2 sublimes. These seasonal actions transport large amounts of dust and water vapor, giving rise to Earth-like frost and large cirrus clouds.

<span class="mw-page-title-main">Gullies on Mars</span> Incised networks of narrow channels and sediments on Mars

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<span class="mw-page-title-main">Planetary surface</span> Where the material of a planetary masss outer crust contacts its atmosphere or outer space

A planetary surface is where the solid or liquid material of certain types of astronomical objects contacts the atmosphere or outer space. Planetary surfaces are found on solid objects of planetary mass, including terrestrial planets, dwarf planets, natural satellites, planetesimals and many other small Solar System bodies (SSSBs). The study of planetary surfaces is a field of planetary geology known as surface geology, but also a focus on a number of fields including planetary cartography, topography, geomorphology, atmospheric sciences, and astronomy. Land is the term given to non-liquid planetary surfaces. The term landing is used to describe the collision of an object with a planetary surface and is usually at a velocity in which the object can remain intact and remain attached.

Nitrogen clathrate or nitrogen hydrate is a clathrate consisting of ice with regular crystalline cavities that contain nitrogen molecules. Nitrogen clathrate is a variety of air hydrates. It occurs naturally in ice caps on Earth, and is believed to be important in the outer Solar System on moons such as Titan and Triton which have a cold nitrogen atmosphere.

<span class="mw-page-title-main">Natural methane on Mars</span>

The reported presence of methane in the atmosphere of Mars is of interest to many geologists and astrobiologists, as methane may indicate the presence of microbial life on Mars, or a geochemical process such as volcanism or hydrothermal activity.

Mars's atmosphere is predominantly composed of CO2 (around 95%) with seasonal air pressure change that facilitates the vaporization and condensation of carbon dioxide. The CO2 cycle on the planet Mars has facilitated the formation of CO2 ice clouds at various locations and seasons on the red planet. Due to low temperatures, especially at Mars's polar caps, carbon dioxide gas can freeze in Mars’s atmosphere to form ice crystallized clouds. Several missions, such as the Viking, Mars Global Surveyor, and Mars Express, have led to interesting observations and measurements regarding CO2 ice clouds. MOLA data in addition to TES spectra have documented ice clouds forming during the winter season of Mars’s northern and southern polar caps. In addition, the Curiosity rover has imaged clouds well above 60 kilometers in the sky at the planet’s equator during the coldest time of Mars’s orbital year (when Mars is furthest away from the Sun due to its elliptical orbit), indicating the possibility of CO2 ice clouds around the planet’s equator. Although further data collection is needed to confirm the formation of CO2 ice clouds on Mars, especially at the planet’s equator, previous measurements have developed a strong argument for frozen carbon dioxide clouds on Mars.

References

  1. ↑ Hassan, Hussein; Zebardast, Soheil; Romanos, Jimmy (2022-09-08). "A Novel Highly Stable Carbon Dioxide Hydrate from a New Synergic Additive Mixture: Experimental and Theoretical Surveys". Journal of Chemical & Engineering Data. 67 (9): 2495–2504. doi:10.1021/acs.jced.2c00239. ISSN   0021-9568.
  2. ↑ Sloan, E. Dendy (1998). Clathrate Hydrates of Natural Gases (2nd ed.). CRC Press. ISBN   978-0-8247-9937-3.[ page needed ]
  3. ↑ Hassan, Hussein; Zebardast, Soheil; Romanos, Jimmy (2022-09-08). "A Novel Highly Stable Carbon Dioxide Hydrate from a New Synergic Additive Mixture: Experimental and Theoretical Surveys". Journal of Chemical & Engineering Data. 67 (9): 2495–2504. doi:10.1021/acs.jced.2c00239. ISSN   0021-9568.
  4. ↑ Fleyfel, Fouad; Devlin, J. Paul (May 1991). "Carbon dioxide clathrate hydrate epitaxial growth: spectroscopic evidence for formation of the simple type-II carbon dioxide hydrate". The Journal of Physical Chemistry. 95 (9): 3811–3815. doi:10.1021/j100162a068.
  5. ↑ Staykova, Doroteya K.; Kuhs, Werner F.; Salamatin, Andrey N.; Hansen, Thomas (1 September 2003). "Formation of Porous Gas Hydrates from Ice Powders: Diffraction Experiments and Multistage Model". The Journal of Physical Chemistry B. 107 (37): 10299–10311. doi:10.1021/jp027787v.
  6. ↑ Kang, Seong-Pil; Lee, Huen (1 October 2000). "Recovery of CO2 from Flue Gas Using Gas Hydrate: Thermodynamic Verification through Phase Equilibrium Measurements". Environmental Science & Technology. 34 (20): 4397–4400. Bibcode:2000EnST...34.4397K. doi:10.1021/es001148l.
  7. ↑ Linga, Praveen; Kumar, Rajnish; Englezos, Peter (19 November 2007). "The clathrate hydrate process for post and pre-combustion capture of carbon dioxide". Journal of Hazardous Materials. 149 (3): 625–629. doi:10.1016/j.jhazmat.2007.06.086. PMID   17689007.
  8. ↑ Babu, Ponnivalavan; Linga, Praveen; Kumar, Rajnish; Englezos, Peter (1 June 2015). "A review of the hydrate based gas separation (HBGS) process for carbon dioxide pre-combustion capture". Energy. 85: 261–279. doi:10.1016/j.energy.2015.03.103.
  9. ↑ Herzog, Howard; Meldon, Jerry; Hatton, Alan (April 2009). Advanced Post-Combustion CO2 Capture (PDF) (Report).
  10. ↑ Wroblewski, Zygmunt Florenty (1882). "Sur la combinaison de l'acide carbonique et de l'eau" [On the combination of carbonic acid and water]. Comptes Rendus de l'Académie des Sciences (in French). 94: 212–213.
  11. ↑ Wroblewski, Zygmunt Florenty (1882). "Sur la composition de l'acide carbonique hydrate" [On the composition of the hydrate of carbonic acid]. Comptes Rendus de l'Académie des Sciences (in French). 94: 254–258.
  12. ↑ Wroblewski, Zygmunt Florenty (1882). "Sur les lois de solubilité de l'acide carbonique dans l'eau sous les hautes pressions" [On the laws of solubility of carbonic acid in water at high pressures]. Comptes Rendus de l'Académie des Sciences (in French). 94: 1355–1357.
  13. ↑ Villard, M. P. (1884). "Sur l'hydrate carbonique et la composition des hydrates de gaz" [On carbonic hydrate and the composition of gas hydrates]. Comptes Rendus de l'Académie des Sciences (in French). Paris. 119: 368–371.
  14. ↑ Villard, M. P. (1897). "Etude expérimentale des hydrates de gaz" [Experimental study of gas hydrates]. Annales de Chimie et de Physique (in French). 11 (7): 289–394.
  15. ↑ Tammann, G.; Krige, G. J. B. (1925). "Die Gleichgewichtsdrucke von Gashydraten" [Equilibrium pressures of gas hydrates]. Zeitschrift für Anorganische und Allgemeine Chemie (in German). 146: 179–195. doi:10.1002/zaac.19251460112.
  16. ↑ Frost, E. M.; Deaton, W. M. (1946). "Gas hydrate composition and equilibrium data". Oil and Gas Journal. 45: 170–178.
  17. ↑ Takenouchi, Sukune; Kennedy, George C. (1 March 1965). "Dissociation Pressures of the Phase CO2 · 5 3/4 H2O". The Journal of Geology. 73 (2): 383–390. doi:10.1086/627068. S2CID   220451948.
  18. ↑ Stackelberg, M. v; Müller, H. R. (1954). "Feste Gashydrate II. Struktur und Raumchemie" [Solid gas hydrates II. Structure and space chemistry]. Zeitschrift für Elektrochemie, Berichte der Bunsengesellschaft für physikalische Chemie (in German). 58 (1): 25–39. doi:10.1002/bbpc.19540580105. S2CID   93862670.
  19. 1 2 Marshall, Michael (26 March 2009). "Ice that burns could be a green fossil fuel". New Scientist.
  20. ↑ "Methane Hydrates Production Field Trial" (PDF). ConocoPhillips. 1 October 2008. Archived from the original (PDF) on 20 November 2008.
  21. ↑ Brewer, Peter G.; Friederich, Gernot; Peltzer, Edward T.; Orr, Franklin M. (7 May 1999). "Direct Experiments on the Ocean Disposal of Fossil Fuel CO2" (PDF). Science. 284 (5416): 943–945. Bibcode:1999Sci...284..943B. doi:10.1126/science.284.5416.943. PMID   10320370. S2CID   43660951. Archived from the original (PDF) on 19 July 2020.
  22. ↑ "NUS research shows CO2 could be stored below ocean floor".
  23. ↑ "Storing carbon under the seafloor could be possible, study explores how". Archived from the original on 2022-03-14. Retrieved 2022-03-15.
  24. ↑ M Fahed, Qureshi; Zheng, Junjie; Khandelwal, Himanshu; Venkatraman, Pradeep; Usadi, Adam; Timothy, Barckholtz; Mhadeshwar, Ashish; Linga, Praveen (Mar 2022). "Laboratory demonstration of the stability of CO2 hydrates in deep-oceanic sediments". Chemical Engineering Journal. 432: 134290. doi:10.1016/j.cej.2021.134290. S2CID   245585287.
  25. 1 2 Miller, Stanley L.; Smythe, William D. (30 October 1970). "Carbon Dioxide Clathrate in the Martian Ice Cap". Science. 170 (3957): 531–533. Bibcode:1970Sci...170..531M. doi:10.1126/science.170.3957.531. PMID   17799706. S2CID   27808378.
  26. ↑ Ross, Russell G.; Kargel, Jeffrey S. (1998). "Thermal Conductivity of Solar System Ices, with Special Reference to Martian Polar Caps". In Schmitt, B.; de Bergh, C.; Festou, M. (eds.). Solar System Ices. Springer. pp. 33–62. doi:10.1007/978-94-011-5252-5_2. ISBN   978-94-011-5252-5.
  27. ↑ Lambert, R.St J.; Chamberlain, V.E. (June 1978). "CO2 permafrost and Martian topography". Icarus. 34 (3): 568–580. Bibcode:1978Icar...34..568L. doi:10.1016/0019-1035(78)90046-5.
  28. 1 2 Hoffman, N (August 2000). "White Mars: A New Model for Mars' Surface and Atmosphere Based on CO2". Icarus. 146 (2): 326–342. Bibcode:2000Icar..146..326H. doi:10.1006/icar.2000.6398.
  29. ↑ Kargel, J. S.; Tanaka, K. L.; Baker, V. R.; Komatsu, G.; Macayeal, D. R. (March 2000). "Formation and Dissociation of Clathrate Hydrates on Mars: Polar Caps, Northern Plains and Highlands". Lunar and Planetary Science Conference: 1891. Bibcode:2000LPI....31.1891K.
  30. ↑ Clifford, Stephen M.; Crisp, David; Fisher, David A.; Herkenhoff, Ken E.; Smrekar, Suzanne E.; Thomas, Peter C.; Wynn-Williams, David D.; Zurek, Richard W.; Barnes, Jeffrey R.; Bills, Bruce G.; Blake, Erik W.; Calvin, Wendy M.; Cameron, Jonathan M.; Carr, Michael H.; Christensen, Philip R.; Clark, Benton C.; Clow, Gary D.; Cutts, James A.; Dahl-Jensen, Dorthe; Durham, William B.; Fanale, Fraser P.; Farmer, Jack D.; Forget, Francois; Gotto-Azuma, Kumiko; Grard, Rejean; Haberle, Robert M.; Harrison, William; Harvey, Ralph; Howard, Alan D.; Ingersoll, Andy P.; James, Philip B.; Kargel, Jeffrey S.; Kieffer, Hugh H.; Larsen, Janus; Lepper, Kenneth; Malin, Michael C.; McCleese, Daniel J.; Murray, Bruce; Nye, John F.; Paige, David A.; Platt, Stephen R.; Plaut, Jeff J.; Reeh, Niels; Rice, James W.; Smith, David E.; Stoker, Carol R.; Tanaka, Kenneth L.; Mosley-Thompson, Ellen; Thorsteinsson, Thorsteinn; Wood, Stephen E.; Zent, Aaron; Zuber, Maria T.; Jay Zwally, H. (1 April 2000). "The State and Future of Mars Polar Science and Exploration". Icarus. 144 (2): 210–242. Bibcode:2000Icar..144..210C. doi:10.1006/icar.1999.6290. PMID   11543391. S2CID   878373.
  31. ↑ Nye, J. F.; Durham, W. B.; Schenk, P. M.; Moore, J. M. (1 April 2000). "The Instability of a South Polar Cap on Mars Composed of Carbon Dioxide". Icarus. 144 (2): 449–455. Bibcode:2000Icar..144..449N. doi:10.1006/icar.1999.6306.
  32. ↑ Jakosky, Bruce M.; Henderson, Bradley G.; Mellon, Michael T. (1995). "Chaotic obliquity and the nature of the Martian climate". Journal of Geophysical Research: Planets. 100 (E1): 1579–1584. Bibcode:1995JGR...100.1579J. doi:10.1029/94JE02801.
  33. ↑ Durham, W. B. (January 1998). "Factors Affecting the Rheologic Properties of Martian Polar Ice". Mars Polar Science and Exploration. 953: 8. Bibcode:1998LPICo.953....8D.
  34. ↑ Musselwhite, Donald S.; Swindle, Timothy D.; Lunine, Jonathan I. (2001). "Liquid CO2 breakout and the formation of recent small gullies on Mars". Geophysical Research Letters. 28 (7): 1283–1285. Bibcode:2001GeoRL..28.1283M. doi: 10.1029/2000GL012496 . S2CID   128618432.
  35. ↑ Max, Michael D.; Clifford, Stephen M. (2001). "Initiation of Martian outflow channels: Related to the dissociation of gas hydrate?". Geophysical Research Letters. 28 (9): 1787–1790. Bibcode:2001GeoRL..28.1787M. doi:10.1029/2000GL011606. S2CID   129028468.
  36. ↑ Pellenbarg, Robert E.; Max, Michael D.; Clifford, Stephen M. (2003). "Methane and carbon dioxide hydrates on Mars: Potential origins, distribution, detection, and implications for future in situ resource utilization". Journal of Geophysical Research: Planets. 108 (E4): 8042. Bibcode:2003JGRE..108.8042P. doi: 10.1029/2002JE001901 .
  37. ↑ McKenzie, Dan; Nimmo, Francis (January 1999). "The generation of martian floods by the melting of ground ice above dykes". Nature. 397 (6716): 231–233. Bibcode:1999Natur.397..231M. doi:10.1038/16649. PMID   9930697. S2CID   4418119.
  38. ↑ Milton, D. J. (15 February 1974). "Carbon Dioxide Hydrate and Floods on Mars". Science. 183 (4125): 654–656. Bibcode:1974Sci...183..654M. doi:10.1126/science.183.4125.654. PMID   17778840. S2CID   26421605.
  39. ↑ Cabrol, N. A.; Grin, E. A.; Landheim, R.; McKay, C. P. (March 1998). "Cryovolcanism as a Possible Origin for Pancake-Domes in the Mars 98 Landing Site Area: Relevance for Climate Reconstruction and Exobiology Exploration" (PDF). Lunar and Planetary Science Conference (1249): 1249. Bibcode:1998LPI....29.1249C.
  40. ↑ Thomas, P.; Squyres, S.; Herkenhoff, K.; Howard, A.; Murray, B. (1992). "Polar deposits of Mars". Mars: 767–795. Bibcode:1992mars.book..767T.
  41. ↑ Kieffer, Hugh H. (10 March 2000). "Clathrates Are Not the Culprit". Science. 287 (5459): 1753b–1753. doi:10.1126/science.287.5459.1753b. S2CID   129784570.
  42. 1 2 3 Stewart, Sarah T.; Nimmo, Francis (2002). "Surface runoff features on Mars: Testing the carbon dioxide formation hypothesis". Journal of Geophysical Research: Planets. 107 (E9): 7–1–7-12. Bibcode:2002JGRE..107.5069S. CiteSeerX   10.1.1.482.6595 . doi:10.1029/2000JE001465.
  43. ↑ Baker, V. R.; Strom, R. G.; Gulick, V. C.; Kargel, J. S.; Komatsu, G. (August 1991). "Ancient oceans, ice sheets and the hydrological cycle on Mars". Nature. 352 (6336): 589–594. Bibcode:1991Natur.352..589B. doi:10.1038/352589a0. S2CID   4321529.
  44. 1 2 Safi, E.; Thompson, S. P.; Evans, A.; Day, S. J.; Murray, C. A.; Parker, J. E.; Baker, A. R.; Oliveira, J. M.; van Loon, J. Th. (5 April 2017). "Properties of CO2 clathrate hydrates formed in the presence of MgSO4 solutions with implications for icy moons". Astronomy & Astrophysics. 600: A88. arXiv: 1701.07674 . Bibcode:2017A&A...600A..88S. doi:10.1051/0004-6361/201629791. S2CID   55958467.
  45. ↑ Sloan, E. Dendy (1998). Clathrate Hydrates of Natural Gases (2nd ed.). CRC Press. ISBN   978-0-8247-9937-3.[ page needed ]
  46. ↑ Genov, Georgi Yordanov (27 June 2005). Physical processes of the CO2 hydrate formation and decomposition at conditions relevant to Mars (Thesis). hdl:11858/00-1735-0000-0006-B57D-6.[ page needed ]
  47. ↑ Sloan, E. Dendy (1998). Clathrate Hydrates of Natural Gases (2nd ed.). CRC Press. ISBN   978-0-8247-9937-3.[ page needed ]
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