A SYSTEMATIC CLASSIFICATION OF METEORITES
PART III

PART I: CHONDRITES, METACHONDRITES
PART II: PRIMITIVE ACHONDRITES, ACHONDRITES, STONY-IRONS, & IRONS

MARTIAN METEORITES

A Geochemical Classification—I
Examples based on Mg# vs. CaO as an indicator for extent of parent magma evolution, and on La–Yb systematics as a measure of enrichment/depletion of the source composition.
Adapted from A. Irving—List of Martian Meteorites

SHERGOTTITES (3 subclasses)
1. ENRICHED SUITE (shallowest source region; variable compositions)
   a. mafic, more evolved (e.g. Los Angeles, Zagami, Shergotty, NWA 3171, NWA 5298, NWA 856, NWA 2800, Dhofar 378 and pairing, NWA 2975 and pairings, JaH 479, Ksar Ghilane 002, NWA 5718, NWA 6963 (Fej Errih) and pairing, NWA 7257, NWA 7320, NWA 10414 [pig-phyric])
   b. permafic, moderately evolved (e.g. NWA 7397, NWA 1068 and pairings, NWA 4468, RBT 04261 and pairing, LAR 06319)
   c. ultramafic, less evolved (or olivine accumulation) (e.g. ALH 84001, NWA 6342)
2. INTERMEDIATE SUITE (Bulk Mars; variable compositions)
   a. mafic, more evolved (e.g. EETA79001B, NWA 480/1460, NWA 5029, NWA 4480 [εHf and εNd indicate unique mantle source plotting between Intermediate and Depleted; Irving et al., 2016, #2330])
   b. permafic, moderately evolved (e.g. EETA79001A, NWA 2646, NWA 6234 and pairings [near primary magma melt], NWA 7042, NWA 2990 and pairings)
   c. ultramafic, less evolved (e.g. ALHA77005 [near primary mantle melt], LEW 88516, GRV 020090, Y-793605, Y-984028 and pairings, Y-1075, GRV 99027, NWA 4797, NWA 10961 [shock veins])
3. DEPLETED SUITE (deepest source region; variable compositions)
   a. mafic, more evolved (e.g. NWA 7635 [after >43% fractional crystallization of Y98-like magma; most depleted shergottite], QUE 94201 [after 43% fractionation], NWA 7635 [olv–plag-phyric], NWA 8159)
   b. permafic, moderately evolved (e.g. Y-980459 and pairing [ol-websterite; near primary mantle melt], NWA 5789 [near primary mantle melt], Dho 019, NWA 2046, NWA 4925, NWA 5990, NWA 7032 and pairing, DaG 476 and pairings, SaU 005 and pairings, NWA 1195, NWA 2626, NWA 4527 and pairing, NWA 6162, Tissint)
   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 ocean crystallization. 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 chassignites, conceivably originating from a deep reservoir, as well as the single known orthopyroxenite 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 REE 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 Silicate Reservoirs on Mars (Wadhwa and Borg, 2006; Papike et al., 2009)
  Trace Elements Redox 147Sm/144Nd ε182W ε142Nd 180Hf/183W
Depleted Mantle
Reservoir 1
LREE Depleted
(shergottites Y-980459,
QUE 94201, DaG 476, SaU 005)
reduced
(IW–IW+1)
≥0.285 ≥0.6 ≥0.9 ≥18
Depleted Mantle
Reservoir 2
LREE Depleted
(nakhlites)
oxidized
(≥IW+3.5)
~0.255–0.266 ~2.95 ~0.74 ~22–43
Depleted Mantle
Reservoir 3
LREE Undepleted
(orthopyroxenite)
reduced
(IW–IW+1)
~0.214 ~0.49 ~0.19 ~19
Enriched Mantle
Reservoir
LREE Enriched
(shergottites Shergotty,
Zagami, LA, NWA 1068)
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 garnet) plus an enriched, trapped, late-stage liquid (after 99.5% crystallization of magma ocean). This stage was followed by cumulate melting which generated partial melts compositionally similar to the most primitive martian meteorites. The other meteorites were generated by fractionation of olivine and orthopyroxene 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 KREEP. 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 melting characteristics and observed incompatible element 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) 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 shergottite 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.


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.
Image credit: A. Treiman and J. Filiberto, Meteoritics & Planetary Science, vol. 50, #4, p. 636 (2015)
'Geochemical diversity of shergottite basalts: Mixing and fractionation, and their relation to Mars surface basalts'

⇒ INCREASING SILICATE FRACTIONATION ⇒
olivine-phyric (3–4.5 wt% Al) low-Al basalt (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

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


PART I: CHONDRITES, METACHONDRITES
PART II: PRIMITIVE ACHONDRITES, ACHONDRITES, STONY-IRONS, & IRONS


You must collect things for reasons you don't yet understand.
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