olivine

Olivine
General
Category	Silicate mineral
Formula; (repeating unit)	(Mg, Fe)2SiO4
Identification
Color	Yellow to yellow-green
Crystal habit	Massive to granular
Crystal system	Orthorhombic
Cleavage	Poor
Fracture	Conchoidal – brittle
Mohs scale hardness	6.5–7
Luster	Vitreous
Streak	White
Diaphaneity	Transparent to translucent
Specific gravity	3.27–3.37
Optical properties	Biaxial (+)
Refractive index	nα = 1.630–1.650; nβ = 1.650–1.670; nγ = 1.670–1.690
Birefringence	δ = 0.040
References

橄欖石　　

WordNet

a mineral consisting of magnesium iron silicate; a source of magnesium

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かんらん石

Wikipedia preview

出典(authority):フリー百科事典『ウィキペディア（Wikipedia）』「2013/01/09 16:23:04」(JST)

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For other uses, see Olivine (disambiguation).

The mineral olivine (when of gem-quality, it is also called peridot and chrysolite), is a magnesium iron silicate with the formula (Mg,Fe)₂SiO₄. It is a common mineral in the Earth's subsurface but weathers quickly on the surface.

The ratio of magnesium and iron varies between the two endmembers of the solid solution series: forsterite (Mg-endmember) and fayalite (Fe-endmember). Compositions of olivine are commonly expressed as molar percentages of forsterite (Fo) and fayalite (Fa) (e.g., Fo₇₀Fa₃₀). Forsterite has an unusually high melting temperature at atmospheric pressure, almost 1900 °C, but the melting temperature of fayalite is much lower (about 1200 °C). The melting temperature varies smoothly between the two endmembers, as do other properties. Olivine incorporates only minor amounts of elements other than oxygen, silicon, magnesium and iron. Manganese and nickel commonly are the additional elements present in highest concentrations.

Olivine gives its name to the group of minerals with a related structure (the olivine group) which includes tephroite (Mn₂SiO₄), monticellite (CaMgSiO₄) and kirschsteinite (CaFeSiO₄).

Identification and paragenesis

Green sand is actually olivine crystals, that have been eroded from lava rocks

Peridotite xenoliths in basalt—olivines are light green crystals. Location: San Carlos Indian Reservation, Gila Co., Arizona, USA.

Lunar olivine basalt collected by Apollo 15.

Olivine is named for its typically olive-green color (thought to be a result of traces of nickel), though it may alter to a reddish color from the oxidation of iron.

Translucent olivine is sometimes used as a gemstone called peridot (péridot, the French word for olivine). It is also called chrysolite (or chrysolithe, from the Greek words for gold and stone). Some of the finest gem-quality olivine has been obtained from a body of mantle rocks on Zabargad island in the Red Sea.

Olivine/peridot occurs in both mafic and ultramafic igneous rocks and as a primary mineral in certain metamorphic rocks. Mg-rich olivine crystallizes from magma that is rich in magnesium and low in silica. That magma crystallizes to mafic rocks such as gabbro and basalt. Ultramafic rocks such as peridotite and dunite can be residues left after extraction of magmas, and typically they are more enriched in olivine after extraction of partial melts. Olivine and high pressure structural variants constitute over 50% of the Earth's upper mantle, and olivine is one of the Earth's most common minerals by volume. The metamorphism of impure dolomite or other sedimentary rocks with high magnesium and low silica content also produces Mg-rich olivine, or forsterite.

Fe-rich olivine is relatively much less common, but it occurs in igneous rocks in small amounts in rare granites and rhyolites, and extremely Fe-rich olivine can exist stably with quartz and tridymite. In contrast, Mg-rich olivine does not occur stably with silica minerals, as it would react with them to form orthopyroxene ((Mg,Fe)₂Si₂O₆).

Mg-rich olivine is stable to pressures equivalent to a depth of about 410 km within Earth. Because it is thought to be the most abundant mineral in Earth’s mantle at shallower depths, the properties of olivine have a dominant influence upon the rheology of that part of Earth and hence upon the solid flow that drives plate tectonics. Experiments have documented that olivine at high pressures (e.g., 12 GPa, the pressure at depths of about 360 kilometers) can contain at least as much as about 8900 parts per million (weight) of water, and that such water contents drastically reduce the resistance of olivine to solid flow; moreover, because olivine is so abundant, more water may be dissolved in olivine of the mantle than contained in Earth's oceans.^[4]

First X-ray view of Martian soil - feldspar, pyroxenes, olivine revealed (Curiosity rover at "Rocknest", October 17, 2012).^[5]

Extraterrestrial occurrences

Mg-rich olivine has also been discovered in meteorites,^[6] the Moon, Mars,^[7] in the dust of comet Wild 2, within the core of comet Tempel 1,^[8] falling into infant stars,^[9] as well as on asteroid 25143 Itokawa.^[10] Such meteorites include chondrites, collections of debris from the early solar system; and pallasites, mixes of iron-nickel and olivine.

The spectral signature of olivine has been seen in the dust disks around young stars. The tails of comets (which formed from the dust disk around the young Sun) often have the spectral signature of olivine, and the presence of olivine has recently been verified in samples of a comet from the Stardust spacecraft.^[11] Comet-like (magnesium-rich) olivine has also been detected in the planetesimal belt around the star Beta Pictoris.^[12]

Crystal structure

Figure 1: The atomic scale structure of olivine looking along the a axis. Oxygen is shown in red, silicon in pink, and magnesium/iron in blue. A projection of the unit cell is shown by the black rectangle

Minerals in the olivine group crystallize in the orthorhombic system (space group Pbnm) with isolated silicate tetrahedra, meaning that olivine is a nesosilicate. In an alternative view, the atomic structure can be described as a hexagonal, close-packed array of oxygen ions with half of the octahedral sites occupied with magnesium or iron ions and one-eighth of the tetrahedral sites occupied by silicon ions.

There are three distinct oxygen sites (marked O1, O2 and O3 in figure 1), two distinct metal sites (M1 and M2) and only one distinct silicon site. O1, O2, M2 and Si all lie on mirror planes, while M1 exists on an inversion center. O3 lies in a general position.

High pressure polymorphs

At the high temperatures and pressures found at depth within the Earth the olivine structure is no longer stable. Below depths of about 410 km (250 mi) olivine undergoes an exothermic phase transition to the sorosilicate, wadsleyite and, at about 520 km (320 mi) depth, wadsleyite transforms exothermically into ringwoodite, which has the spinel structure. At a depth of about 660 km (410 mi), ringwoodite decomposes into silicate perovskite ((Mg,Fe)SiO₃) and ferropericlase ((Mg,Fe)O) in an endothermic reaction. These phase transitions lead to a discontinuous increase in the density of the Earth's mantle that can be observed by seismic methods. They are also thought to influence the dynamics of mantle convection in that the exothermic transitions reinforce flow across the phase boundary, whereas the endothermic reaction hampers it.^[13]

The pressure at which these phase transitions occur depends on temperature and iron content.^[14] At 800 °C (1,070 K; 1,470 °F), the pure magnesium end member, forsterite, transforms to wadsleyite at 11.8 gigapascals (116,000 atm) and to ringwoodite at pressures above 14 GPa (138,000 atm). Increasing the iron content decreases the pressure of the phase transition and narrows the wadsleyite stability field. At about 0.8 mole fraction fayalite, olivine transforms directly to ringwoodite over the pressure range 10.0–11.5 GPa (99,000–113,000 atm). Fayalite transforms to Fe₂SiO₄ spinel at pressures below 5 GPa (49,000 atm). Increasing the temperature increases the pressure of these phase transitions.

Weathering

Olivine weathering to iddingsite within a mantle xenolith

Olivine is one of the weaker common minerals on the surface according to the Goldich dissolution series. It weathers to iddingsite (a combination of clay minerals, iron oxides and ferrihydrites) readily in the presence of water.^[15] The presence of iddingsite on Mars would suggest that liquid water once existed there, and might enable scientists to determine when there was last liquid water on the planet.^[16]

Uses

A worldwide search is on for cheap processes to sequester CO₂ by mineral reactions. Removal by reactions with olivine is an attractive option, because it is widely available and reacts easily with the (acid) CO₂ from the atmosphere. When olivine is crushed, it weathers completely within a few years, depending on the grain size. All the CO₂ that is produced by burning 1 liter of oil can be sequestered by less than 1 liter of olivine. The reaction is exothermic but slow. In order to recover the heat produced by the reaction to produce electricity, a large volume of olivine must be thermally well-isolated. The end-products of the reaction are silicon dioxide, magnesium carbonate and small amounts of iron oxide.^[17]^[18]

The aluminium foundry industry uses olivine sand to cast objects in aluminium. Olivine sand requires less water than silica sands while still holding the mold together during handling and pouring of the metal. Less water means less gas (steam) to vent from the mold as metal is poured into the mold.^[19]

References

^ Olivine. Webmineral.com Retrieved on 2012-06-16.
^ Olivine. Mindat.org Retrieved on 2012-06-16.
^ Klein, Cornelis; and C. S. Hurlburt (1985). Manual of Mineralogy (21st ed.). New York: John Wiley & Sons. ISBN 0-471-80580-7.
^ Smyth, J. R.; Frost, D. J.; Nestola, F.; Holl, C. M.; Bromiley, G. (2006). "Olivine hydration in the deep upper mantle: Effects of temperature and silica activity". Geophysical Research Letters 33 (15). Bibcode 2006GeoRL..3315301S. doi:10.1029/2006GL026194.
^ Brown, Dwayne (October 30, 2012). "NASA Rover's First Soil Studies Help Fingerprint Martian Minerals". NASA. http://www.nasa.gov/home/hqnews/2012/oct/HQ_12-383_Curiosity_CheMin.html. Retrieved October 31, 2012.
^ Fukang and other Pallasites. Farlang.com (2008-04-30). Retrieved on 2012-06-16.
^ Pretty Green Mineral.... Planetary Science Research Discoveries, Hawaii Institute of Geophysics and Planetology
^ Mission Update 2006... UMD Deep Impact Website, University of Maryland Ball Aerospace & Technology Corp. retrieved June 1, 2010
^ Spitzer Sees Crystal Rain... NASA Website
^ Japan says Hayabusa brought back asteroid grains... retrieved November 18, 2010
^ Press Release 06-091. Jet Propulsion Laboratory Stardust website, retrieved May 30, 2006.
^ De Vries, B. L.; Acke, B.; Blommaert, J. A. D. L.; Waelkens, C.; Waters, L. B. F. M.; Vandenbussche, B.; Min, M.; Olofsson, G. et al. (2012). "Comet-like mineralogy of olivine crystals in an extrasolar proto-Kuiper belt". Nature 490 (7418): 74–76. doi:10.1038/nature11469. PMID 23038467. edit
^ Christensen, U.R. (1995). "Effects of phase transitions on mantle convection". Ann. Rev. Earth Planet. Sci. 23: 65–87. Bibcode 1995AREPS..23...65C. doi:10.1146/annurev.ea.23.050195.000433.
^ Deer, W. A.; R. A. Howie, and J. Zussman (1992). An Introduction to the Rock-Forming Minerals (2nd ed.). London: Longman. ISBN 0-582-30094-0.
^ Kuebler, K.; Wang, A.; Haskin, L. A.; Jolliff, B. L. (2003). "A Study of Olivine Alteration to Iddingsite Using Raman Spectroscopy". Lunar and Planetary Science 34: 1953. http://www.lpi.usra.edu/meetings/lpsc2003/pdf/1953.pdf.
^ Swindle, T. D.; Treiman, A. H.; Lindstrom, D. J.; Burkland, M. K.; Cohen, B. A.; Grier, J. A.; Li, B.; Olson, E. K. (2000). "Noble Gases in Iddingsite from the Lafayette meteorite: Evidence for Liquid water on Mars in the last few hundred million years". Meteoritics and Planetary Science 35 (1): 107–115. Bibcode 2000M&PS...35..107S. doi:10.1111/j.1945-5100.2000.tb01978.x.
^ Philip Goldberg, Zhong-ying Chen, William O Connor, Richard Walters, Hans Ziock (2000). "CO2 Mineral Sequestration Studies in US". Technology 1 (1): 1–10. http://www.netl.doe.gov/publications/proceedings/01/carbon_seq/6c1.pdf.
^ Schuiling, R. D.; Krijgsman, P. (2006). "Enhanced Weathering: An Effective and Cheap Tool to Sequester Co2". Climatic Change 74: 349–354. doi:10.1007/s10584-005-3485-y.
^ Ammen, C.W. (1980). The Metal Caster's Bible. Blue Ridge Summit PA: TAB. p. 331. ISBN 0-8306-9970-8.

External links

Pretty Green Mineral – Pretty Dry Mars? by Linda M.V. Martel, Planetary Science Research Discoveries, Hawai'i Institute of Geophysics and Planetology
Olivine Page Farlang library: Historic sources + modern articles on Olivine and Peridot
Geological information and several microscopic images University of North Dakota

English Journal

Chemical and morphological changes during olivine carbonation for CO2 storage in the presence of NaCl and NaHCO3.

Gadikota G, Matter J, Kelemen P, Park AH.Author information Department of Chemical Engineering, Columbia University in the City of New York, New York, NY 10027, USA.AbstractThe increasing concentrations of CO2 in the atmosphere are attributed to the rising consumption of fossil fuels for energy generation around the world. One of the most stable and environmentally benign methods of reducing atmospheric CO2 is by storing it as thermodynamically stable carbonate minerals. Olivine ((Mg,Fe)2SiO4) is an abundant mineral that reacts with CO2 to form Mg-carbonate. The carbonation of olivine can be enhanced by injecting solutions containing CO2 at high partial pressure into olivine-rich formations at high temperatures, or by performing ex situ mineral carbonation in a reactor system with temperature and pressure control. In this study, the effects of NaHCO3 and NaCl, whose roles in enhanced mineral carbonation have been debated, were investigated in detail along with the effects of temperature, CO2 partial pressure and reaction time for determining the extent of olivine carbonation and its associated chemical and morphological changes. At high temperature and high CO2 pressure conditions, more than 70% olivine carbonation was achieved in 3 hours in the presence of 0.64 M NaHCO3. In contrast, NaCl did not significantly affect olivine carbonation. As olivine was dissolved and carbonated, its pore volume, surface area and particle size were significantly changed and these changes influenced subsequent reactivity of olivine. Thus, for both long-term simulation of olivine carbonation in geologic formations and the ex situ reactor design, the morphological changes of olivine during its reaction with CO2 should be carefully considered in order to accurately estimate the CO2 storage capacity and understand the mechanisms for CO2 trapping by olivine.
Physical chemistry chemical physics : PCCP.Phys Chem Chem Phys.2014 Feb 12;16(10):4679-93. doi: 10.1039/c3cp54903h.
The increasing concentrations of CO2 in the atmosphere are attributed to the rising consumption of fossil fuels for energy generation around the world. One of the most stable and environmentally benign methods of reducing atmospheric CO2 is by storing it as thermodynamically stable carbonate mineral
PMID 24469156

B3LYP Periodic Study of the Physico-Chemical Properties of the Non-Polar (010) Mg-Pure and Fe-Containing Olivine Surfaces.

Navarro-Ruiz J, Ugliengo P, Rimola A, Sodupe M.AbstractB3LYP periodic simulations have been carried out to study some physico-chemical properties of the bulk structures and the corresponding non-polar (010) surfaces of Mg-pure and Fe-containing olivine systems; i.e, Mg2SiO4 (Fo) and Mg1.5Fe0.5SiO4 (Fo75). A detailed structural analysis of the (010) Fo and Fo75 surface models shows the presence of coordinatively unsaturated metal cations (Mg2+ and Fe2+, respectively) with shorter metal-O distances compared to the bulk ones. Energetic analysis devoted to the Fe2+ electronic spin configuration and to the ion position in the surfaces reveals that Fe2+ in its quintet state and placed at the outermost positions of the slab constitutes the most stable Fe-containing surface, which is related to the higher stability of high spin states when Fe2+ is coordinatively unsaturated. Comparison of the simulated IR and the corresponding reflectance spectra indicates that Fe2+ substitution induces an overall bathochromic shift of the spectra due to the larger mass of Fe compared to Mg cation. In contrast, the IR spectra of the surfaces are shifted to upper values and exhibit more bands compared to the corresponding bulk systems due to the shorter metal-O distances given in the coordinatively unsaturated metals and to symmetry reduction which brings non-equivalent motions between the outermost and the internal modes, respectively.
The journal of physical chemistry. A.J Phys Chem A.2014 Feb 11. [Epub ahead of print]
B3LYP periodic simulations have been carried out to study some physico-chemical properties of the bulk structures and the corresponding non-polar (010) surfaces of Mg-pure and Fe-containing olivine systems; i.e, Mg2SiO4 (Fo) and Mg1.5Fe0.5SiO4 (Fo75). A detailed structural analysis of the (010) Fo a
PMID 24517343

Catalytic reforming of toluene as tar model compound: Effect of Ce and Ce-Mg promoter using Ni/olivine catalyst.

Zhang R1, Wang H2, Hou X2.Author information 1Institute of Chemistry and Molecular Engineering & Research Institute of Environmental Sciences, Zhengzhou University, PR China; Key Lab of Environmental Chemistry and Low Carbon Technologies of Henan Province, Zhengzhou 450052, PR China. Electronic address: rqzhang@zzu.edu.cn.2Institute of Chemistry and Molecular Engineering & Research Institute of Environmental Sciences, Zhengzhou University, PR China; Key Lab of Environmental Chemistry and Low Carbon Technologies of Henan Province, Zhengzhou 450052, PR China.AbstractTar produced by biomass gasification as a route of renewable energy must be removed before the gas can be used. This study was undertaken using toluene as a model tar compound for evaluating its steam reforming conversion with three Ni-based catalysts, Ni/olivine, Ni-Ce/olivine and Ni-Ce-Mg/olivine. Effects of Ce and Mg promoters on the reaction activity and coke deposition were studied. Overall the performance of Ce and Mg promoted Ni/olivine catalysts is better than that of only Ce promoter and Ni/olivine alone. The experimental results indicate that Ni-Ce-Mg/olivine catalysts could improve the resistance to carbon deposition, enhance energy gases yield and resist 10ppm H2S poison at 100mLmin(-1) for up to 400min. Furthermore, the activity of catalysts was related to the steam/carbon (S/C) ratios; at S/C ratio=5, T=790°C, space velocity=782h(-1) and t=2h, the Ni-Ce-Mg/olivine system yielded 89% toluene conversion, 5.6Lh(-1) product gas rate, 62.6mol% H2 content and 10% (mol useful gas mol(-1) toluene) energy yield. Moreover, at low S/C ratio, it had higher reaction activity and better ability to prevent coking. There is a small amount of carbon deposition in the form of amorphous carbon after 7h. Various characterization techniques such as XRD, FTIR and thermogravimetric were performed to investigate the coke deposition of Ni/olivine, Ni-Ce/olivine and Ni-Ce-Mg/olivine. It is suggested that 3% Ni-1% Ce-1% Mg/olivine was the most promising catalyst due to its minimum coke amount and the lower activation energy of coke burning.
Chemosphere.Chemosphere.2014 Feb;97:40-6. doi: 10.1016/j.chemosphere.2013.10.087. Epub 2013 Nov 22.
Tar produced by biomass gasification as a route of renewable energy must be removed before the gas can be used. This study was undertaken using toluene as a model tar compound for evaluating its steam reforming conversion with three Ni-based catalysts, Ni/olivine, Ni-Ce/olivine and Ni-Ce-Mg/olivine.
PMID 24275153

Japanese Journal

Relationship between CAIs and chondrules: A case study of a compound chondrule from the Allende (CV3) meteorite

ＧＥＯＣＨＥＭＩＣＡＬ　ＪＯＵＲＮＡＬ 51(1), 31-43, 2017
NAID 130005317105

Constraints on mechanisms of chondrule formation from chondrule precursors and chronology of transient heating events in the protoplanetary disk

ＧＥＯＣＨＥＭＩＣＡＬ　ＪＯＵＲＮＡＬ 51(1), 45-68, 2017
NAID 130005317082

Evidence for the solar wind in lunar magmas: A study of slowly cooled samples of the Apollo 12 olivine basalt suite

ＧＥＯＣＨＥＭＩＣＡＬ　ＪＯＵＲＮＡＬ 51(1), 95-104, 2017
NAID 130005317080

Related Pictures

[1] Olivine. Webmineral.com Retrieved on 2012-06-16.

[2] Olivine. Mindat.org Retrieved on 2012-06-16.

[3] Klein, Cornelis; and C. S. Hurlburt (1985). Manual of Mineralogy (21st ed.). New York: John Wiley & Sons. ISBN 0-471-80580-7.

[4] Smyth, J. R.; Frost, D. J.; Nestola, F.; Holl, C. M.; Bromiley, G. (2006). "Olivine hydration in the deep upper mantle: Effects of temperature and silica activity". Geophysical Research Letters 33 (15). Bibcode 2006GeoRL..3315301S. doi:10.1029/2006GL026194.

[NASA-20121030-5] Brown, Dwayne (October 30, 2012). "NASA Rover's First Soil Studies Help Fingerprint Martian Minerals". NASA. http://www.nasa.gov/home/hqnews/2012/oct/HQ_12-383_Curiosity_CheMin.html. Retrieved October 31, 2012.

[6] Fukang and other Pallasites. Farlang.com (2008-04-30). Retrieved on 2012-06-16.

[7] Pretty Green Mineral.... Planetary Science Research Discoveries, Hawaii Institute of Geophysics and Planetology

[8] Mission Update 2006... UMD Deep Impact Website, University of Maryland Ball Aerospace & Technology Corp. retrieved June 1, 2010

[9] Spitzer Sees Crystal Rain... NASA Website

[10] Japan says Hayabusa brought back asteroid grains... retrieved November 18, 2010

[11] Press Release 06-091. Jet Propulsion Laboratory Stardust website, retrieved May 30, 2006.

[deVries2012-12] De Vries, B. L.; Acke, B.; Blommaert, J. A. D. L.; Waelkens, C.; Waters, L. B. F. M.; Vandenbussche, B.; Min, M.; Olofsson, G. et al. (2012). "Comet-like mineralogy of olivine crystals in an extrasolar proto-Kuiper belt". Nature 490 (7418): 74–76. doi:10.1038/nature11469. PMID 23038467. edit

[13] Christensen, U.R. (1995). "Effects of phase transitions on mantle convection". Ann. Rev. Earth Planet. Sci. 23: 65–87. Bibcode 1995AREPS..23...65C. doi:10.1146/annurev.ea.23.050195.000433.

[14] Deer, W. A.; R. A. Howie, and J. Zussman (1992). An Introduction to the Rock-Forming Minerals (2nd ed.). London: Longman. ISBN 0-582-30094-0.

[15] Kuebler, K.; Wang, A.; Haskin, L. A.; Jolliff, B. L. (2003). "A Study of Olivine Alteration to Iddingsite Using Raman Spectroscopy". Lunar and Planetary Science 34: 1953. http://www.lpi.usra.edu/meetings/lpsc2003/pdf/1953.pdf.

[16] Swindle, T. D.; Treiman, A. H.; Lindstrom, D. J.; Burkland, M. K.; Cohen, B. A.; Grier, J. A.; Li, B.; Olson, E. K. (2000). "Noble Gases in Iddingsite from the Lafayette meteorite: Evidence for Liquid water on Mars in the last few hundred million years". Meteoritics and Planetary Science 35 (1): 107–115. Bibcode 2000M&PS...35..107S. doi:10.1111/j.1945-5100.2000.tb01978.x.

[17] Philip Goldberg, Zhong-ying Chen, William O Connor, Richard Walters, Hans Ziock (2000). "CO2 Mineral Sequestration Studies in US". Technology 1 (1): 1–10. http://www.netl.doe.gov/publications/proceedings/01/carbon_seq/6c1.pdf.

[18] Schuiling, R. D.; Krijgsman, P. (2006). "Enhanced Weathering: An Effective and Cheap Tool to Sequester Co2". Climatic Change 74: 349–354. doi:10.1007/s10584-005-3485-y.

[19] Ammen, C.W. (1980). The Metal Caster's Bible. Blue Ridge Summit PA: TAB. p. 331. ISBN 0-8306-9970-8.

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