Systematics: Martian Meteorites – Geochemical Classification

PART I: CHONDRITES, METACHONDRITES
PART II: PRIMITIVE ACHONDRITES, ACHONDRITES, STONY-IRONS, IRONS
PART IV: DIOGENITES—IUGS TAXONOMY
PART V: ENSTATITE CHONDRITES—SUBGROUP CLASSIFICATION

MARTIAN METEORITES

A Geochemical Classification—I
Examples based on Mg# vs. CaO as an indicator for extent of parent magmaMolten silicate (rock) beneath the surface of a planetary body or moon. When it reaches the surface, magma is called lava. evolution, and on La–Yb systematics as a measure of enrichment/depletion of the source composition.
Adapted from A. Irving—List of Martian Meteorites

SHERGOTTITESIgneous stony meteorite with a Martian origin consisting mainly of plagioclase (or a shocked glass of plagioclase composition) and pyroxene. They are the most abundant type of SNC meteorites and the type member is the Shergotty meteorite, which fell in India in 1865. Shergottites are igneous rocks of volcanic or (3 subclasses)

1. ENRICHED SUITE (shallowest source region; variable compositions)

a. mafic, more evolved (e.g. Dhofar 378 and pairing, JaH 479, Ksar Ghilane 002, Los Angeles, NWA 856, NWA 2800, NWA 2975 and pairings, NWA 3171, NWA 5298, NWA 5718, NWA 6963 (Fej Errih) and pairing, NWA 7257, NWA 7320, NWA 10414 [pig-phyric], Shergotty, Zagami)

b. permafic, moderately evolved (e.g. NWA 1068 and pairings [poss. near primary mantleMain silicate-rich zone within a planet between the crust and metallic core. The mantle accounts for 82% of Earth's volume and is composed of silicate minerals rich in Mg. The temperature of the mantle can be as high as 3,700 °C. Heat generated in the core causes convection currents in melt of intermediate Mg# along with LAR 06319], NWA 4468, NWA 7397, RBT 04261/62)

c. ultramaficTerm used for silicate minerals with cations predominantly Mg and/or Fe. Mafic minerals are dominated by plagioclase and pyroxene, and also contain smaller amounts of olivine., less evolved (or olivineGroup of silicate minerals, (Mg,Fe)2SiO4, with the compositional endpoints of forsterite (Mg2SiO4) and fayalite (Fe2SiO4). Olivine is commonly found in all chondrites within both the matrix and chondrules, achondrites including most primitive achondrites and some evolved achondrites, in pallasites as large yellow-green crystals (brown when terrestrialized), in the silicate portion accumulation) (e.g. ALH 84001)

2. INTERMEDIATE SUITE (Bulk Mars; variable compositions)

a. mafic, more evolved (e.g. EETA79001B, NWA 480/1460, NWA 4480 [εHf and εNd indicate unique mantle source plotting between Intermediate and Depleted; Irving et al., 2016, #2330], NWA 5029)

b. permafic, moderately evolved (e.g. EETA79001A, NWA 1950, NWA 2646, NWA 2990 and pairings, NWA 6234 and pairings [near primary magma melt], NWA 7042, NWA 10169, NWA 11065, NWA 11214)

c. ultramafic, less evolved (e.g. ALHA77005 [near primary mantle melt], GRV 99027, GRV 020090, LEW 88516, NWA 4797, NWA 6342, NWA 10697, NWA 10961 [shock veins], NWA 11261, Y-1075, Y-793605, Y-984028 and pairings)

3. DEPLETED SUITE (deepest source region; variable compositions)

a. mafic, more evolved (e.g. NWA 7635 [olv–plag-phyric; after >43% fractional crystallizationA crystallization process in which minerals crystallizing from a magma are isolated from contact with the liquid. It is a key process in the formation of igneous rocks during the process of magmatic differentiation. Also known as crystal fractionation. of Y98-like magma; most depleted shergottite], NWA 8159 [near primary mantle melt], QUE 94201 [after 43% fractionation])

b. permafic, moderately evolved (e.g. DaG 476 and pairings, Dho 019, NWA 1195, NWA 2046, NWA 2626, NWA 4527 and pairing, NWA 4925, NWA 5789 [near primary mantle melt], NWA 5990, NWA 6162, NWA 7032 and pairing, SaU 005 and pairings, Tissint, Y-980459 and pairing [ol-websterite; near primary mantle melt])

c. ultramafic, less evolved (sample unknown)

According to Papike et al. (2009), both depleted and enriched material were formed early in the planet’s history as a result of magma oceanCompletely molten surfaces of terrestrial planets or moons that formed soon after accretion. Samples returned by the Apollo missions provide evidence of a lunar magma ocean, crystallization of which produced a stratified Moon with a low-density crust formed by accumulation of the mineral plagioclase overlying a higher density mantle of crystallizationPhysical or chemical process or action that results in the formation of regularly-shaped, -sized, and -patterned solid forms known as crystals.. Although complex two- and three-stage petrogenetic models have been proposed, martian lithologies can be resolved into four basic reservoirs based on geochemical, isotopic, and mineralogical characteristics. These reservoirs represent the shergottites through contrasting models: one involving mantle magma assimilation of crustal material, and another, perhaps more plausible, involving the mixing of multiple mantle magma reservoirs linked by fractional crystallization. These four basic reservoirs also represent the nakhlites and chassignitesThe group is part of the SNC martian trio and named after the meteorite seen to fall in Chassigny, France, in 1815. Its subsequent recovery led to it being one of the first meteorites to be recognized as a genuine rock from space. Chassigny resembles a terrestrial dunite - a, conceivably originating from a deep reservoir, as well as the single known orthopyroxeniteA rock composed primarily of orthopyroxene. Non-terrestrial orthopyoxenites include diogenites and a single martian meteorite, ALH 84001, that was found in the Allan Hills region of Antarctica in 1984. ALH 84001 is a cumulate rock consisting of 97% coarse-grained, Mg-rich orthopyroxene, with small amounts of plagioclase, chromite, and carbonate. It ALH 84001, conceivably originating from a shallow reservoir.

Although ALH 84001 is an orthopyroxenite, and as such was characterized by the Planetary Chemistry Laboratory at Washington University as a subgroup of the nakhlites, its parental source magma has a composition that is consistent with the same mixtures of depleted and enriched REEOften abbreviated as “REE”, these 16 elements include (preceded by their atomic numbers): 21 scandium (Sc), 39 Yttrium (Y) and the 14 elements that comprise the lanthanides excluding 61 Promethium, an extremely rare and radioactive element. These elements show closely related geochemical behaviors associated with their filled 4f atomic orbital. end-member components that are used in a geochemical classification of the shergottites (Lapen et al., 2012). It was determined that the source magma of ALH 84001 contained a higher proportion of the enriched REE component than all other shergottites studied thus far. Therefore, ALH 84001 might be most appropriately classified as a subgroup of the shergottites.

The four basic reservoirs distinguished by Papike et al. (2009) are shown in the following table:

Comparison of Four SilicateThe most abundant group of minerals in Earth's crust, the structure of silicates are dominated by the silica tetrahedron, SiO44-, with metal ions occurring between tetrahedra). The mesodesmic bonds of the silicon tetrahedron allow extensive polymerization and silicates are classified according to the amount of linking that occurs between the Reservoirs on Mars (Wadhwa and Borg, 2006; Papike et al., 2009)

	Trace Elements	RedoxOxidation and reduction together are called redox (reduction and oxidation) and generally characterized by the transfer of electrons between chemical species, like molecules, atoms or ions, where one species undergoes oxidation, a loss of electrons,  while another species undergoes reduction, a gain of electrons. This transfer of electrons between reactants	147Sm/144Nd	ε182W	ε142Nd	180Hf/183W
Depleted Mantle Reservoir 1	LREE Depleted (shergottites DaG 476, QUE 94201, SaU 005, Y-980459)	reducedOxidation and reduction together are called redox (reduction and oxidation) and generally characterized by the transfer of electrons between chemical species, like molecules, atoms or ions, where one species undergoes oxidation, a loss of electrons,  while another species undergoes reduction, a gain of electrons. This transfer of electrons between reactants (IW–IW+1)	≥0.285	≥0.6	≥0.9	≥18
Depleted Mantle Reservoir 2	LREE Depleted (nakhlites)	oxidizedOxidation and reduction together are called redox (reduction and oxidation) and generally characterized by the transfer of electrons between chemical species, like molecules, atoms or ions, where one species undergoes oxidation, a loss of electrons,  while another species undergoes reduction, a gain of electrons. This transfer of electrons between reactants (≥IW+3.5)	~0.255–0.266	~2.95	~0.74	~22–43
Depleted Mantle Reservoir 3	LREE Undepleted (orthopyroxenite ALH 84001)	reduced (IW–IW+1)	~0.214	~0.49	~0.19	~19
Enriched Mantle Reservoir	LREE Enriched (shergottites Los Angeles, NWA 1068, Shergotty, Zagami)	oxidized (>IW+2)	<0.182	≤0.3	≤–0.2	≤11

A new hybridized model developed by Borg and Draper (2003) suggests that the martian magma ocean crystallized and produced a depleted mantle (45% opx, 38% ol, 14% cpx, and 3% majoritic garnetMineral generally found in terrestrial metamorphic rocks, although igneous examples are not uncommon. Garnet is a significant reservoir of Al in the Earth's upper mantle. The garnet structure consists of isolated SiO4 tetrahedra bound to two cation sites. The A site holds relatively large divalent cations (Ca2+, Mg2+, Fe2+, Mn2+); the) plus an enriched, trapped, late-stage liquid (after 99.5% crystallization of magma ocean). This stage was followed by cumulateIgneous rock composed of crystals that have grown and accumulated (often by gravitational settling) in a cooling magma chamber. melting which generated partial melts compositionally similar to the most primitive martian meteorites. The other meteorites were generated by fractionationConcentration or separation of one mineral, element, or isotope from an initially homogeneous system. Fractionation can occur as a mass-dependent or mass-independent process. of olivine and orthopyroxeneOrthorhombic, low-Ca pyroxene common in chondrites. Its compositional range runs from all Mg-rich enstatite, MgSiO3 to Fe-rich ferrosilite, FeSiO3. These end-members form an almost complete solid solution where Mg2+ substitutes for Fe2+ up to about 90 mol. % and Ca substitutes no more than ~5 mol. % (higher Ca2+ contents occur to form parental melts in initial conditions of high pressure (≥12 GPa), superchondritic CaO/AlO ratio, high Mg# (~80), and an FeO component of ~13.5 wt%. The late-stage liquid was trapped in the cumulate pile after 98–99.5% crystallization, representing a component analogous to lunar KREEPLunar igneous rock rich in potassium (K), rare-earth elements (REE), phosphorus (P), thorium, and other incompatible elements. These elements are not incorporated into common rock-forming minerals during magma crystallization, and become enriched in the residual magma and the rocks that ultimately crystallize from it. (potassium–rare earth element–phosphorus). Basaltic martian meteorites were derived from the melting of mixtures of cumulates and late-stage liquids that crystallized ~4.5 b.y. ago.

The above hybridized model was refined by Lapen et al. (2010) to describe the mantle source of shergottites as well as the orthopyroxenite ALH 84001. Their model generally agrees with that of Borg and Draper (2003), which propounds that the various martian lithologies were produced from variable mixtures of depleted cumulate material and trapped, enriched residual liquids; however, improved age and isotopic data indicate that residual liquid remaining after ~93–98% crystallization of the magma ocean was not part of the mixture that produced enriched shergottites. The average mixture of the shergottites was determined to consist of 94% cumulates and 6% trapped residual liquids, and the depth of the mantle reservoir—consistent with partial meltingAn igneous process whereby rocks melt and the resulting magma is comprised of the remaining partially melted rock (sometimes called restite) and a liquid whose composition differs from the original rock. Partial melting occurs because nearly all rocks are made up of different minerals, each of which has a different melting characteristics and observed incompatible elementSubstance composed of atoms, each of which has the same atomic number (Z) and chemical properties. The chemical properties of an element are determined by the arrangement of the electrons in the various shells (specified by their quantum number) that surround the nucleus. In a neutral atom, the number of abundances—was calculated to be 250–400 km. The research team recognized two distinct mantle reservoirs: one in which the shergottites and ALH 84001 were formed, and another in which the nakhlites were formed.

Nonetheless, Andreasen et al. (2015, #2976) demonstrated that a three-component mixing model for martian mantle source regions remains as the most consistent given the growing amount of isotopic data from an increasing number of shergottiteIgneous stony meteorite with a Martian origin consisting mainly of plagioclase (or a shocked glass of plagioclase composition) and pyroxene. They are the most abundant type of SNC meteorites and the type member is the Shergotty meteorite, which fell in India in 1865. Shergottites are igneous rocks of volcanic or analyses. These are described as a depleted reservoir with high Sm/Nd and high Lu/Hf ratios, a depleted reservoir with high Sm/Nd and low Lu/Hf ratios, and an enriched reservoir with low Sm/Nd and Lu/Hf ratios. The known shergottites presently encompass virtually the entire range of mantle compositions established in the three-component mixing model, delineated by the depleted end-member NWA 7635 and the enriched end-member ALH 84001. Such a three-component mixing model involving depleted, enriched, and KREEP-like end-members is supported by the results of a statistical analysis based on Sr-Nd-Hf-Pb isotopes in shergottites conducted by Jean and Taylor (2017, #1666).

A Geochemical Classification—II
Examples based on elemental abundance ratios under a hypothesis for a two-component mixing relationship coupled with silicate fractionation and/or olivine accumulation among shergottites.
Table credit: A. Treiman and J. Filiberto, MAPS, vol. 50, #4, p. 636 (2015)
‘Geochemical diversity of shergottite basalts: Mixing and fractionation, and their relation to Mars surface basalts’ (http://dx.doi.org/10.1111/maps.12363)

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⇒ INCREASING SILICATE FRACTIONATION ⇒
olivine-phyric (3–4.5 wt% Al)	low-Al basaltBasalt is the most common extrusive igneous rock on the terrestrial planets. For example, more than 90% of all volcanic rock on Earth is basalt. The term basalt is applied to most low viscosity dark silicate lavas, regardless of composition. Basalt is a mafic, extrusive and fine grained igneous rock (3–4.5 wt% Al)	high-Al basalt (5–6.5 wt% Al)
*NWA 1068 (enriched)	Zagami (enriched)	*Los Angeles (enriched)
Y-980459 (depleted)	Shergotty (enriched)	QUE 94201 (depleted)
LAR 06319(enriched)	NWA 856 (enriched)	Dhofar 378 (enriched)
NWA 6234 (intermediate)	NWA 480/1460 (intermediate)	EETA79001B (intermediate)
EETA79001A (intermediate)	NWA 5298 (enriched)	Ksar Ghilane 002 (enriched)
Dag 476/489 (depleted)
SaU 005 (depleted)
Tissint (depleted)
NWA 5789 (depleted)

* The crystallization ages for the evolutionary endmember couple NWA 1068/Los Angeles are consistent with a direct magma source relationship. The geochemical diversity among the martian basalts was examined by Treiman and Filiberto (2015), and a new model of petrogenesis was proposed. Utilizing elemental abundance ratios (primarily involving incompatible elements, but also Al and Ni), they divided the pyroxene-phyric and olivine-phyric shergottites into three subgroups in order of increasing evolution: olivine-phyric ⇒ low-Al basalt ⇒ high-Al basalt. They reasoned that an evolutionary relationship exists between these subgroups, and asserted that the diversity among them occurred as a result of differential mixing of two primary magma (or source) components—one depleted and the other enriched in incompatible elements. The enriched component was described as a highly evolved product of fractionation of a magma ocean analogous to lunar KREEP. Further processing followed the mixing stage, which involved variable degrees of silicate fractionation and/or accumulation of olivine megacrysts. Although the full range of geochemical variability of the martian basalt meteorites may be represented in our present collections, a third complementary mixing component hypothesized to exist could still be missing.

Classification schemes and data for this page were adapted from the following sources: Borg and Draper, 2003
Warren and Bridges, 2005
Irving et al., 2007
Symes et al., 2008
Bunch et al., 2008
Irving and Kuehner, 2008
Shih et al., 2009
Rumble III and Irving, 2009
Papike et al., 2009
Irving et al., 2010
Lapen et al., 2010
Treiman and Filiberto, 2014
Andreasen et al., 2015
Jean and Taylor, 2017

A more in-depth treatment of the classification of martian meteorites can be found on Dr. Anthony Irving’s Martian Meteorites website.

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PART I: CHONDRITES, METACHONDRITES
PART II: PRIMITIVE ACHONDRITES, ACHONDRITES, STONY-IRONS, IRONS
PART IV: DIOGENITES—IUGS TAXONOMY
PART V: ENSTATITE CHONDRITES—SUBGROUP CLASSIFICATION

You must collect things for reasons you don’t yet understand.
Daniel J. Boorstin – Librarian of Congress

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