Numerous fragments of 4 Vesta were ejected by collisions one and two billion years ago that left two enormous craters occupying much of Vesta's southern hemisphere.[1][2] Debris from these events has fallen to Earth as howardite–eucrite–diogenite (HED) meteorites, which have been a rich source of information about Vesta.[3][4][5]

A 175 g individual of the Millbillillie meteorite shower, an eucrite achondrite, fell in Australia in 1960. Credit: H. Raab.{{free media}}

Vesta's Greek equivalent is Hestia.[6] Minerals likely to have originated on the asteroid 4 Vesta may be called Hestiominerals.

V asteroids Edit

Location and structure of the Vesta family are depicted. Credit: Deuar.
As NASA's Dawn spacecraft takes off for its next destination, this mosaic synthesizes some of the best views the spacecraft had of the giant asteroid Vesta. Credit: NASA/JPL-Caltech/UCAL/MPS/DLR/IDA.{{free media}}

In the full image of Vesta at right, the rocky-object appears to have suffered from meteor damage.

As NASA's Dawn spacecraft took off for its next destination, this mosaic synthesizes some of the best views the spacecraft had of the giant asteroid Vesta. Dawn studied Vesta from July 2011 to September 2012. The towering mountain at the south pole — more than twice the height of Mount Everest — is visible at the bottom of the image. The set of three craters known as the "snowman" can be seen at the top left.

Vesta, minor-planet designation 4 Vesta, is one of the largest asteroids in the Solar System. It lost some 1% of its mass less than a billion years ago in a collision that left an enormous crater occupying much of its southern hemisphere. Debris from this event has fallen to Earth as howardite–eucrite–diogenite (HED) meteorites, a rich source of information about the asteroid.[4][5]

"V-type asteroids are bodies whose surfaces are constituted of basalt. In the Main Asteroid Belt, most of these asteroids are assumed to come from the basaltic crust of Asteroid (4) Vesta."[7]

The Vestian asteroids consist "of 4 Vesta, the second-most-massive of all asteroids (mean diameter of 530 km), and many small asteroids below 10 km diameter. The brightest of these, 1929 Kollaa and 2045 Peking, have an absolute magnitude of 12.2, which would give them a radius of about 7.5 km assuming the same high albedo as 4 Vesta."[8]

"A [Hierarchical Clustering Method] (HCM) numerical analysis (by Zappala 1995) determined a large group of 'core' family members, whose proper orbital elements lie in the approximate ranges"[8]

ap ep ip
min 2.26 AU 0.075 5.6°
max 2.48 AU 0.122 7.9°

"This gives the approximate boundaries of the family. At the present epoch, the range of  osculating orbital elements of these core members is"[8]

a e i
min 2.26 AU 0.035 5.0°
max 2.48 AU 0.162 8.3°

"The Zappala 1995 analysis[9] found 235 core members. A search of a recent proper-element database (AstDys) for 96944 minor planets in 2005 yielded 6051 objects (about 6% of the total) lying within the Vesta-family region as per the first table above."[8]

Howardite–eucrite–diogenite meteorites Edit

"Approximately 1,700 HED meteorites have been identified in the meteorite collections; however, high-pressure minerals have only been reported in one shocked eucrite18."[10]

"Using Dawn’s Gamma Ray and Neutron Detector, [elemental mapping on Vesta has been accomplished.] Global Fe/O and Fe/Si ratios are consistent with [howardite, eucrite, and diogenite] HED [meteorite] compositions."[11]

Diogenites Edit

The Johnstown diogenite mineral sample is shown. Credit: NASA.{{free media}}

Def. an "achondritic stony meteorite originating from deep within the crust of the asteroid 4 Vesta"[12] is called a diogenite.

Diogenites are composed of igneous rocks of plutonic origin, having solidified slowly enough deep within Vesta's crust to form crystals which are larger than in the eucrites, which are primarily magnesium-rich orthopyroxene (enstatite), with small amounts of plagioclase and olivine.[13]

"The remaining six are interpreted as diogenitic in composition and were designated as J asteroids (mnemonic for the Johnstown diogenite)."[14]

Eucrites Edit

NWA 3359 meteorite is a eucrite, where here the full slice is 3.6 cm across at its widest. Credit: James St. John.{{free media}}

Def. an "achondritic meteoritic rock consisting chiefly of pigeonite and anorthite"[15] is called a eucrite.

The eucrite specimen at top right is approximately 6 cm wide. Note the shiny black fusion crust with flow lines. The chip at lower right allows one to see the light-gray interior. The orange staining at top is a result of weathering, as these stones were not recovered until many years after they fell.

Eucrites consist of basaltic rock from the crust of 4 Vesta or a similar parent body, mostly composed of Ca-poor pyroxene, pigeonite, and Ca-rich plagioclase (anorthite).[16]

NWA 8003 Edit

"[T]issintite, vacancy-rich clinopyroxene, and super-silicic garnet in the eucrite Northwest Africa (NWA) 8003 [combined] with coesite and stishovite, the presence of these high-pressure minerals and their chemical compositions reveal that solidification of melt veins in NWA 8003 began at a pressure of >~10 GPa and ceased when the pressure dropped to <~8.5 GPa."[10]

Howardites Edit

This 2.74 g crusted slice contains a large eucrite clast as well as diogenitic fragments making an interesting matrix. Credit: Jon Taylor.{{free media}}

Def. an "achondritic stony meteorite"[17] is called a howardite.

"High precision spectrophotometry of 4 Vesta, the third largest asteroid, was used to establish the surface composition of this body and to investigate mineralogical variations across its surface."[18]

"The average surface of Vesta is analogous to howardite and/or polymict eucrite assemblages, regolith-derived members of the HED meteorite suite which consist of a eucrite matrix containing differing amounts of a diogenite component."[18]

"Color and/or spectral changes, which exhibit a consistent relationship to rotational phasing, are evident in 16 of 18 studies of Vesta dating back to 1929, including the present work. After elimination of possible sources of spurious spectral or color changes, it is concluded that these variations arise from hemispheric variations in surface materials, and hence provide a means of spatially resolving subhemispheric compositional units on the surface of Vesta."[18]

"The background surface of Vesta is a relatively dark howardite or polymict eucrite (pyroxene–plagioclase) assemblage with several compositionally distinct bright regions clustered in one hemisphere viewed around the maximum in Vesta's lightcurve. These include what appears to be an olivine-bearing unit (suggested name “Leslie Formation”) located near Vesta's equator which probably represents an impact basin (and/or its associated ejecta) that penetrated through the basaltic crust. Other high-albedo compositional units including an apparently low-calcium eucrite region and several diogenite (pyroxenite) regions, at least one located near the southern pole, may be smaller, shallower impact basins."[18]

"By analogy to the eucrite meteorites, which represent surface flows or shallow intrusions and which constitute the major component of the regolith-derived howardites and polymict eucrites, [...] the howardite/polymict eucrite units represent a regolith-gardened original surface of Vesta. It is probable that the low albedo of the background surface on Vesta is due to an age-related darkening effect similar to that inferred from the Galileo images of Gaspra and Ida. This mechanism is consistent with the correlation of absorption feature intensity with the lightcurve. Vesta appears to have an old eucritic surface, darkened with age and represented among the meteorites by the regolith-derived howardites and polymict eucrites, on which several impacts on one hemisphere have exposed fresher brighter diogenite and olivine-bearing material."[18]

"Based on qualitative analysis of the mineralogical variations as a function of rotation, a generalized lithologic map of Vesta was produced. There is reasonable control on the longitude of lithologic features but little control on their latitudes, except where specifically noted. In producing this map, discrete circular features were used on the plausible assumption that impacts have been the most important geologic process on this surface for most of the age of the solar system. The shape of the features has thus been assumed rather than derived and is subject to future revision as data improve."[18]

Maskelynites Edit

NWA 1195 is a Martian meteorite composed largely of maskelynite. Credit: Jon Taylor.{{free media}}
A photomicrograph of a plagioclase crystal under cross polarized light, where the plagioclase crystal shows a distinct banding effect called polysynthetic twinning. Credit: Chmee2.{{free media}}

Maskelynite was first identified in the Shergotty meteorite by Gustav Tschermak von Seysenegg (1872) as an isotropic glass of an unknown origin with near labradorite composition.[19] Similar phases were found in chondrites and Martian meteorites. In 1963, D. J. Milton and P. S. de Carli produced a maskelynite-like glass by subjecting gabbro to an explosive shock wave.[20]

"Maskelynite occurs in the rocks of the central peaks of Clearwater West and Manicouagan craters, Quebec, Canada."[21]

"A clear, glassy pseudomorph of plagioclase was described in the Shergotty basaltic achondrite by Tschermak (1872) and named maskelynite."[21]

Maskelynite is "a transformation of plagioclase produced by remelting or by mechanical means."[21]

"A mechanical transformation of Stillwater gabbro to a rock resembling shergottite was achieved by Milton and DeCarli (1963) by shock-loading the gabbro at 250 to 350 kb peak pressure and a calculated temperature of no more than 350°C. They advocated restricting the term maskelynite to a non-crystalline phase clearly pseudomorphous after crystalline feldspar. Duke (1963) restudied the Shergotty meteorite in detail and suggested the maskelynite resulted from a passage of a strong shock wave through the meteorite."[21]

"Terrestrial samples containing isotropic material conforming to Milton and DeCarli's definition have been collected from two large probable ancient meteorite craters in the Canadian Shield (Beals, et al. 1963)."[21]

Plagioclase is a series of tectosilicate minerals within the feldspar group with a specific chemical composition: NaAlSi
. Plagioclase in hand samples is often identified by its polysynthetic crystal twinning or 'record-groove' effect.

Analysis of thermal emission spectra from the surface of Mars suggests that plagioclase is the most abundant mineral in the crust of Mars.[22]

Anorthites Edit

Anorthite crystals are in a basalt vug from Vesuvius. Credit: Robert M. Lavinsky.{{free media}}

Anorthites have the chemical formula CaAl

Anorthite is rare on the Earth[24] but abundant on the Moon.[25]

Anorthite is a rare compositional variety of plagioclase that occurs in mafic igneous rock, also occurs in metamorphic rocks of granulite facies, in metamorphosed carbonate rocks, and corundum deposits,[26] type localities are Monte Somma and Valle di Fassa, Italy. It was first described in 1823,[27] more rare in surficial rocks than it normally would be due to its high weathering potential in the Goldich dissolution series.

It also makes up much of the lunar highlands; the Genesis Rock, collected during the 1971 Apollo 15 mission, is made of anorthosite, a rock composed largely of anorthite. Anorthite was discovered in samples from comet Wild 2, and the mineral is an important constituent of Ca-Al-rich inclusions in rare varieties of chondritic meteorites.

Augites Edit

Augite is a black, single-chain inosilicate mineral, a pyroxene. Credit: Didier Descouens.{{free media}}

Formula: (Ca
, where 0.4 ≤ x ≤ 0.9, x+y+z=1 and y1+z1=1.[28]

IMA Formula: (Ca,Mg,Fe)

Crystal System: Monoclinic, Clinopyroxene Subgroup > Pyroxene Group.[28]

Common Impurities: Ti,Cr,Na,Mn,K.[28]

Geological Setting: Major rock forming mineral in mafic igneous rocks, ultramafic rocks, and some high-grade metamorphic rocks.[28]

Augite is an essential mineral in mafic igneous rocks; for example, gabbro and basalt and common in ultramafic rocks, occurs in relatively high-temperature metamorphic rocks such as mafic granulite and metamorphosed iron formations, commonly occurs in association with orthoclase, sanidine, labradorite, olivine, leucite, amphiboles and other pyroxenes.[29]

Clinopyroxenes Edit

"A subgroup name for monoclinic Pyroxene Group minerals."[30]

"The most widespread members include aegirine, augite, hedenbergite and diopside."[30]

"In the Ca-Fe-Mg (diopside-hedenbergite-augite) quadrilateral, the ideal structural formula is M2M1[Si
], where M2 is a distorted octahedral site which preferentially accepts large cations such as alkaline earth/alkali atoms (Ca, but may accept transition metals) and where M1 is a smaller regular octahedral site preferentially accepting transition metals, etc. (most commonly Mg, Fe2+
). The substitutions containing no changes in valence within M2 (2+), Mi (2+), and tetrahedral sites, T (4+), is the normal scheme. A variety of additional substitution schemes, which require coupling of substituents, have been identified in these pyroxenes. Often these substitutions result in a change of species designation when they are dominant."[28]

"Substitution 1 has Na substitution in M2 and trivalent ions of Al, Fe, Cr, and Sc substituting in M1."[28]

"Substitution 2 involves Na substitution in M2 and mixed valance transition metals such as [Fe2+
] substituting in M1."[28]

"Substitution 3, also called Tschermak's Component, involves coupled M1 octahedral and tetrahedral substitutions, such as CaAl[AlSiO
] or CaTi3+

"Substitution 4 is a variant of Substitution 2 and has dominant Ca in M2 with mixed valence substitution in M1 involving divalent and tetravalent Ti and Al substitution in tetrahedral sites, e.g. Ca[(Mg, Fe2+
]. In highly substituted Ca-Fe-Mg pyroxenes, several substitutional schemes may be identified."[28]

"Substitution schemes 2 and 4 have not yet yielded named mineral species."[28]

"Augite could be considered to be a sub-calcic member of the diopside-hedenbergite series but, as defined by Morimoto et al. (1988) may have Fe>Mg or Mg>Fe without a change in name. Because of the way augite has been defined (Morimoto et al, 1988), there is the implication that in rare cases, a variety of anions may be dominant in various the various sites, including M2, M1, and T. These extreme compositions are rare in the large majority of augites. The clinopyroxenes with Wo
are classed as pigeonite, another mineral that could be thought of as slightly alkalic clinoenstatite-clinoferrosilite."[28]

"However, there is a structural discontinuity between these pyroxenes at low-medium temperatures, and detailed chemical analysis and even structural analysis should be obtained in order to properly classify these unusual compositions. Similarly, extensive substitution of Na, for example, as in scheme 1 (Morimoto et al., 1988) could lead to Aegirine-augite or aegirine compositions depending on the other elements involved."[28]

Coesites Edit

Crossed-polars image of coesite grain (gray) ~1 mm across is in eclogite, small colored inclusion is pyroxene, polycrystalline rim is quartz. Credit: J. Smyth.{{free media}}
Atomic structure is of coesite. Credit: Materialscientist.{{free media}}

Coesite is a polymorph of silicon dioxide SiO
that is formed when very high pressure (2–3 gigapascals), and moderately high temperature (700 °C, 1,300 °F), are applied to quartz. Coesite was first synthesized by Loring Coes Jr., a chemist at the Norton Company, in 1953.[31][32]

In 1960, a natural occurrence of coesite was reported by Edward C. T. Chao,[33] in collaboration with Eugene Shoemaker, from the Barringer Crater, in Arizona, US, which was evidence that the crater must have been formed by an impact. After this report, the presence of coesite in unmetamorphosed rocks was taken as evidence of a meteorite impact event or of an atomic bomb explosion. It was not expected that coesite would survive in high pressure metamorphic rocks.

In metamorphic rocks, coesite was initially described in eclogite xenoliths from the mantle of the Earth that were carried up by ascending magmas; kimberlite is the most common host of such xenoliths.[34] In metamorphic rocks, coesite is now recognized as one of the best mineral indicators of metamorphism at very high pressures (UHP, or ultrahigh-pressure metamorphism).[35] Such UHP metamorphic rocks record subduction or continental collisions in which crustal rocks are carried to depths of 70 km (43 mi) or more. Coesite is formed at pressures above about 2.5 GPa (25 kbar) and temperature above about 700 °C. This corresponds to a depth of about 70 km in the Earth. It can be preserved as mineral inclusions in other phases because as it partially reverts to quartz, the quartz rim exerts pressure on the core of the grain, preserving the metastable grain as tectonic forces uplift and expose these rock at the surface. As a result, the grains have a characteristic texture of a polycrystalline quartz rim.

Coesite has been identified in UHP metamorphic rocks around the world, including the western Alps of Italy at Dora Maira,[35] the Erzgebirge of Germany,[36] the Lanterman Range of Antarctica,[37] in the Kokchetav Massif of Kazakhstan,[38] in the Western Gneiss region of Norway,[39] the Dabie-Shan Range in Eastern China,[40] the Himalayas of Eastern Pakistan,[41] and the Vermont Appalachian Mountains.[42][43]

Coesite is a tectosilicate with each silicon atom surrounded by four oxygen atoms in a tetrahedron. Each oxygen atom is then bonded to two Si atoms to form a framework. There are two crystallographically distinct Si atoms and five different oxygen positions in the unit cell. Although the unit cell is close to being hexagonal in shape ("a" and "c" are nearly equal and β nearly 120°), it is inherently monoclinic and cannot be hexagonal. The crystal structure of coesite is similar to that of feldspar and consists of four silicon dioxide tetrahedra arranged in Si
and Si
rings. The rings are further arranged into chains. This structure is metastable within the stability field of quartz: coesite will eventually decay back into quartz with a consequent volume increase, although the metamorphic reaction is very slow at the low temperatures of the Earth's surface. The crystal symmetry is monoclinic C2/c, No.15, Pearson symbol mS48.[44]

Enstatites Edit

Enstatite is from the Bare Hills Copper Mine (Smith Avenue Copper Mine), Bare Hills, Baltimore County, Maryland, USA. Credit: Robert M. Lavinsky.{{free media}}
  1. Formula: Mg
  2. Crystal System: Orthorhombic.[45]
  3. Class (H-M): mmm (2/m 2/m 2/m) - Dipyramidal.[45]
  4. Space Group: Pbca.[45]
  5. Cell Parameters: a = 18.23 Å, b = 8.84 Å, c = 5.19 Å.[45]
  6. Z: 8.[45]
  7. Polymorph of: Akimotoite, Bridgmanite, Clinoenstatite.[45]
  8. Hardness: 5 - 6 on Mohs scale.[45]
  9. Tenacity: Brittle.[45]
  10. Common Impurities: Fe,Ca,Al,Co,Ni,Mn,Ti,Cr,Na,K.[45]

Enstatite and the other orthorhombic pyroxenes are distinguished from those of the monoclinic series by their optical characteristics, such as straight extinction, much weaker double refraction and stronger pleochroism.[46]

The "enstatite achondrite-like E-asteroids almost certainly derive from the melting and differentiation of highly reduced parent materials analogous to enstatite chondrites (e.g., Keil 1989)."[47]

Garnets Edit

This is pyrope garnet from Madagaskar. Credit: Stowarzyszenie Spirifer.{{free media}}

"Abundances of rare earth elements, Hf, Sc, Co, Cr and Th in garnet megacrysts and their volcanic hosts or matrices are used to estimate garnet/liquid partition coefficients for these elements."[48]

"The wide variation in garnet/liquid partition coefficients from kimberlites to rhyolites cannot be explained as an effect of temperature and we conclude that a major factor is the composition of the melt from which the garnet crystallized."[48]

"Garnet = Mineral Group of general formula: A3B2(SiO4)3, A = Ca, Mg, Fe2+, Mn2+; B = Al, Fe3+, Cr, V, Zr, Ti."[49]

The garnets make up two solid solution series: pyrope-almandine-spessartine (pyralspite), with the composition range [Mg,Fe,Mn]
; and uvarovite-grossular-andradite (ugrandite), with the composition range Ca

Def. a "hard transparent mineral that is often used as gemstones and abrasives"[50] is called a garnet.

"Back-scattered electron image of a typically zoned shock melt vein in NWA 8003 [shows] Cpx: clinopyroxene; Grt: garnet; Coe: coesite; Cpx: clinopyroxene; FSA: fine-grained silica aggregate.[10]

"Garnet occurs as fine dendritic or anhedral to euhedral grains in the zoned melt veins of NWA 8003 [...]."[10]

"Electron Probe Micro-Analyzer (EPMA) results [...] reveal that all garnets are super-silicic, containing 6–13 mol% majorite components [Mg
]. The garnet grains within the eclogitic mineral assemblage contain slightly higher Si concentrations (3.09–3.13 atoms per formula unit, apfu; based on 12 analyses) than those in the central zone (3.06–3.09 apfu, 9 analyses), based on 12 oxygen atoms. In contrast, the Al concentrations in the former (1.70–1.80 apfu) are slightly lower than those in the latter (1.77–1.83 apfu)."[10]

Olivines Edit

This image is a visual close up of green sand which is actually olivine crystals that have been eroded from lava rocks. Credit: Brocken Inaglory.{{free media}}
This is a visual image of a forsterite crystal. Credit: Azuncha.{{free media}}

Def. "[a]ny of a group of olive green magnesium-iron" orthosilicates "that crystallize in the orthorhombic system"[51] is called an olivine.

At right is a visual close up of green sand which is actually olivine crystals that have been eroded from lava rocks. Some olivine crystals are still inside the lava rock.

Forsterite "(Mg2SiO4) is the magnesium rich end-member of the olivine solid solution series."[52]

"Forsterite is associated with igneous and metamorphic rocks and has also been found in meteorites. In 2005 it was also found in cometary dust returned by the Stardust probe.[53] In 2011 it was observed as tiny crystals in the dusty clouds of gas around a forming star.[54]"[52]

"Two polymorphs of forsterite are known: wadsleyite (also orthorhombic) and ringwoodite (isometric). Both are mainly known from meteorites."[52]

Orthopyroxenes Edit

A sample of orthopyroxenite is from meteorite ALH84001 from Mars. Credit: the USGS (Specific photographer credit not given at source.{{free media}}

Pyroxenes that crystallize in the orthorhombic system are known as orthopyroxenes, e.g.:

  • Enstatite, Mg
  • Bronzite, intermediate between enstatite and hypersthene
  • Hypersthene, (Mg,Fe)SiO
  • Eulite, intermediate between hypersthene and ferrosilite
  • Ferrosilite, Fe
  • Donpeacorite, (MgMn)MgSi
  • Nchwaningite, Mn2+

Pigeonites Edit

Polarized light microscope image of part of a grain of orthopyroxene containing exsolution lamellae of augite. Credit: Omphacite.{{free media}}

In the image on the right is a polarized light microscope image of part of a grain of orthopyroxene containing exsolution lamellae of augite from the Bushveld intrusion. The texture documents a multistage history: (1) crystallization of twinned pigeonite, followed by exsolution of augite; (2) breakdown of pigeonite to orthopyroxene plus augite; (3) exsolution of augite parallel to the former twin plane of pigeonite.

Formula: (Ca,Mg,Fe)(Mg,Fe)Si
. The calcium cation fraction can vary from 5% to 25%, with iron and magnesium making up the rest of the cations.

Pigeonite is a mineral in the clinopyroxene subgroup of the pyroxene group.

Pigeonite is found as phenocrysts in volcanic rocks on Earth and as crystals in meteorites from Mars and the Moon. In slowly cooled intrusive igneous rocks, pigeonite is rarely preserved. Slow cooling gives the calcium the necessary time to separate itself from the structure to form exsolution lamellae of calcic clinopyroxene[55], leaving no pigeonite present.[56] Textural evidence of its breakdown to orthopyroxene plus augite may be present, as shown in the accompanying microscopic image.

Pigeonite is named for its type locality on Lake Superior's shores at Pigeon Point, Minnesota, United States. It was first described in 1900.[57][58]

Quartzes Edit

This is a sample from a hydrothermal quartz (white)-gold vein (Precambrian) of the Archean Cadillac Group in southwestern Quebec, Canada. Credit: James St. John.{{free media}}

Red "thermoluminescence (RTL) emission from quartz, as a dosimeter for baked sediments and volcanic deposits, [from] older (i.e., >1 Ma), quartz-bearing known age volcanic deposits [can use as standards] independently-dated silicic volcanic deposits from New Zealand, ranging in age from 300 ka through to 1.6 Ma."[59]

"Back-scattered electron images of high-pressure minerals in NWA 8003 [show a] quartz grain adjacent to a melt vein has transformed to stishovite and silica glass."[10]

Stishovites Edit

Crystal structure is of stishovite. Credit: Materialscientist.{{free media}}

Stishovite is an extremely hard, dense tetragonal polymorph of silicon dioxide. It is very rare on the Earth's surface; however, it may be a predominant form of silicon dioxide in the Earth, especially in the lower mantle.[60]

Stishovite was named after Sergey M. Stishov, a Russian high-pressure physicist who first synthesized the mineral in 1961. It was discovered in Meteor Crater in 1962 by Edward C. T. Chao.[61]

Unlike other silica polymorphs, the crystal structure of stishovite resembles that of rutile TiO
. The silicon in stishovite adopts an octahedral coordination geometry, being bound to six oxides. Similarly, the oxides are three-connected, unlike low-pressure forms of SiO2. In most silicates, silicon is tetrahedral, being bound to four oxides.[62] It was long considered the hardest known oxide (~30 GPa Vickers[63]); however, boron suboxide has been discovered[64] in 2002 to be much harder. At normal temperature and pressure, stishovite is metastable.

Stishovite can be separated from quartz by applying hydrogen fluoride (HF); unlike quartz, stishovite will not react.[61]

Large natural crystals of stishovite are extremely rare and are usually found as clasts of 1 to 2 mm in length. When found, they can be difficult to distinguish from regular quartz without laboratory analysis. It has a vitreous luster, is transparent (or translucent), and is extremely hard. Stishovite usually sits as small rounded gravels in a matrix of other minerals.

Until recently, the only known occurrences of stishovite in nature formed at the very high shock pressures (>100 kbar, or 10 GPa) and temperatures (> 1200 °C) present during hypervelocity meteorite impact into quartz-bearing rock. Minute amounts of stishovite have been found within diamonds,[65] and post-stishovite phases were identified within ultra-high-pressure mantle rocks.[66] Stishovite may also be synthesized by duplicating these conditions in the laboratory, either isostatically or through shock (see shocked quartz).[67] At 4.287 g/cm3, it is the second densest polymorph of silica, after seifertite. It has tetragonal crystal symmetry, P42/mnm, No. 136, Pearson symbol tP6.[68]

Def. a polymorph of α-quartz formed by pressures > 100 kbar or 10 GPa and temperatures > 1200 °C is called stishovite.[69]

Stishovite may be formed by an instantaneous over pressure such as by an impact or nuclear explosion type event.[70]

Minute amounts of stishovite has been found within diamonds.[65]

Tissintites Edit

Back-scattered electron images of tissintite occurs in maskelynite adjacent to shock-melt veins. Credit: Run-Lian Pang, Ai-Cheng Zhang, Shu-Zhou Wang, Ru-Cheng Wang & Hisayoshi Yurimoto.{{free media}}

"The high-pressure minerals tissintite [Tst], vacancy-rich clinopyroxene [Cpx], and super-silicic garnet are observed in the shocked eucrite Northwest Africa (NWA) 8003 in addition to coesite and stishovite."[10]

In the image on the right are "Cpx: clinopyroxene; Opx: orthopyroxene; Aug: augite; Tro: troilite; Msk: maskelynite; Tst: tissintite; FSA: fine-grained silica aggregate."[10] "It consists dominantly of clinopyroxene with minor mineral fragments and fine-grained silica aggregates."[10]

"Based on six oxygen atoms, the tissintite in NWA 8003 has an average chemical formula (Ca
with high vacancy concentrations [□0.27] on the M2 site."[10]

Troilites Edit

Polished and etched surface of the Mundrabilla meteorite from Australia is shown, where the darker brownish areas with striations are troilite with exolved daubréelite. Credit: Raymond T. Downward, NASA.{{free media}}

This is a macro photograph of an etched surface of the Mundrabilla meteorite, a small piece of the approximately 3.9 billion-year-old meteorite that was first discovered in Western Australia in 1911. Two more giant chunks, together weighing about 17 tons, were found in 1966. Researchers can learn much from this natural crystal growth experiment since it has spent several hundred million years cooling, and would be impossible to emulate in a lab. This single slice, taken from a 6 ton piece recovered in 1966, measures only 2 square inches. The macro photograph shows a metallic iron-nickel alloy phase of kamcite (38% Ni) and taenite (6% Ni) at bottom right, bottom left, and top left. The darker material is an iron sulfide (FeS or troilite) with parallel precipitates of duabreelite (iron chromium sulfide (FeCr

See Also Edit

References Edit

  1. Jutzi, M.; E. Asphaug; P. Gillet; J.-A. Barrat; W. Benz (14 February 2013). "The structure of the asteroid 4 Vesta as revealed by models of planet-scale". Nature 494 (7436): 207–210. doi:10.1038/nature11892. PMID 23407535. 
  2. Cook, Jia-Rui. "Dawn Reality-Checks Telescope Studies of Asteroids". Retrieved 30 April 2014. {{cite web}}: |archive-date= requires |archive-url= (help)
  3. McSween, H. Y.; R. P. Binzel; M. C. De Sanctis; E. Ammannito; T. H. Prettyman; A. W. Beck; V. Reddy; L. Le Corre et al. (27 November 2013). "Dawn; the Vesta-HED connection; and the geologic context for eucrite, diogenites, and howardites". Meteoritics & Planetary Science 48 (11): 2090–21–4. doi:10.1111/maps.12108. 
  4. 4.0 4.1 Kelley, M. S. (2003). "Quantified mineralogical evidence for a common origin of 1929 Kollaa with 4 Vesta and the HED meteorites". Icarus 165 (1): 215–218. doi:10.1016/S0019-1035(03)00149-0. 
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