Miller Range 03346, 090030, 090032, and 090136 715.2, 452 ...2 O (as OH groups). Mineral Chemistry...

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Miller Range 03346, 090030, 090032, and 090136 715.2, 452.6, 532.5, 171 grams

Nakhlites

Figure 1: Four paired nakhlites from the Miller Range (MIL), Transantarctic Mountains; clockwise from

upper left – MIL 03346, MIL 090030, MIL 090032, and MIL 090136

Introduction

A large (~715 g) nakhlite – the first in the US Antarctic meteorite collection - was

discovered Dec 15, 2003 in the Miller Range of the Transantarctic Mountains. About 60

% of the surface of MIL 03346 was covered with black, shiny wrinkled fusion crust

(Figure 1). MIL 03346 is a nakhlite with abundant clinopyroxene and rare olivine set in a

fine-grained mesostasis with some alteration (Righter and Satterwhite, 2004). Several

years later, the 2009-2010 ANSMET team recovered three additional nakhlite samples

that were quickly realized to be paired with MIL 03346 – MIL 090030, 090032, and

090136. These additional pairs are also sizable, and the combined mass of the pairing

group is nearly 2 kg. These samples have provided new constraints on the source of the

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nakhlites, the associated petrology of their setting on Mars, and many other aspects of the

geologic, geochemical, and geophysical evolution of Mars.

Figure 2: Portion of the Miller Range where nakhlites were found.

Petrography

MIL 03346 and pairs (pairing group abbreviated as MIL in the rest of this write-up) is a

cumulate of abundant elongate clinopyroxene (0.2 to 2.5 mm) and minor olivine crystals

(up to 1.7 mm) set in a dark-colored, fine-grained intercumulate mesostasis (Stopar et al.

2005; McKay and Schwandt 2005; Mikouchi et al. 2005; Rutherford et al. 2005; Day et

al. 2006 and Imae and Ikeda 2007). Stopar et al. and Day et al. compared the grain size

distribution of MIL with that of the other clinopyroxenites, finding that it had the largest

average crystal size (0.43 x 0.26 mm).

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Figure 3: Photomicrographs of MIL nakhlites

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Early work on the modal mineralogy of MIL 03346 revealed its mesostasis-rich nature

(20-35%; Figure 4; Stopar et al., 2005; Rutherford et al. (2005); McKay and Schwandt,

2005; Anand et al., 2005; Mikouchi et al. 2005; Day et al., 2006; Ikeda, 2007).

Comparison of the textures and mineralogy of the paired masses have been carried out by

Corrigan et al., (2015), Udry et al., (2012), and Hallis et al. (2013), and appear in Table 1.

The higher fraction of mesostasis in MIL 03346 compared to Nakhla is evident in Figure

5.

Figure 4: X-ray chemical map of MIL 03346, illustrating the distribution of major and minor

minerals and the relatively large fraction of mesostasis (from Stopar et al., 2008).

Figure 5: ternary plot of modal % olivine, pyroxene, and mesostasis in MIL nakhlites

compared to Nakhla (from Corrigan et al., 2015).

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From Udry et al. (2012)

The mesostasis (Figure 6) consists of a dendritic intergrowth of fayalite, ferro-

hedenbergite, Ti-magnetite, cristobalite, apatite and feldspar glass (like that of NWA

817). No plagioclase has been found in MIL. Day et al. (2005, 2006) conclude that MIL

is part of the same cumulate-rich lava flow as the other nakhlites, but that it experienced

less equilibration and faster cooling than the other nakhlites.

Magmatic melt inclusions (Figure 7) are reported in the olivine (Rutherford et al. 2005)

and in augite (Imae and Ikeda 2007; Ikeda, 2005). Various phases, including jarosite,

saponite and Cl-rich amphibole, have been reported in these melt inclusions (McCubbin

et al. 2008; Imae and Ikeda 2007; Sautter et al. 2006). Imae and Ikeda (2007) calculate

the composition of the trapped (parental) magma from these melt inclusions.

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Figure 6 (left): SEM image of mesostasis

Figure 7 (right): magmatic melt inclusion in olivine

Olivine has “iddingsite-smectite” alteration in cracks, like that found in the other

nakhlites (Arnand et al. 2005; Stopar et al. 2005). Mikouchi et al. (2005) note that the

alteration in MIL 03346 (Antarctica) is like that in NWA 817 (Sahara Desert) and that

this might indicate the alteration is pre-terrestrial. Stopar et al. (2005) report that

“gypsum is found in cracks, voids and veins throughout the thin sections.” Sautter et al.

(2005, 2007) report Cl-rich amphibole, chlorite, phosphate and a “mixed sulfate of Fe and

S” which they interpret as derived from a soil component on Mars. Day et al. (2006)

found that this alteration assemblage in MIL 03346 is probably a sub-micrometer mixture

of smectite clay, iron oxy-hydroxides and salt minerals, with up to 14 wt. % H2O (as OH

groups).

Mineral Chemistry

Olivine: MIL has less olivine (3%) than the other nakhlites (Day et al. 2006). McKay

and Schwandt (2005) found that large olivine grains (up to 1.7 mm) have uniform cores

Fo44-43, but zone to Fo5 at their outer rims. Range of olivine reported from MIL pairs and

other nakhlites is shown in Figure 8. Tiny skeletal fayalite is found in the mesostasis.

Pyroxenes: Cores of clinopyroxene cluster around Wo39En27. The rim zone increases in

Fe and decreases in Ca to ~Wo34En14. Mikouchi et al. (2005), Anand et al. (2005) and

McKay and Schwandt (2005) found that the outer rims, adjacent to the mesostasis, zone

to ferro-hedenbergite (Figure 8). Imae and Ikeda found that the outer rims of pyroxene

phenocrysts contain up to 10 wt.% Al2O3. Domeneghetti et al. (2006) found the iron in

MIL was oxidized (Fe+3). The full range of reported clinopyroxene compositions is

shown in Figure 8, along with comparisons to other nakhlites (Udry et al., 2012).

Ti-magnetite: Dendritic chains of Ti-magnetite are prevalent in the mesostasis (like

NWA 817). Day et al. (2006) determined that magnetite was chemically zoned from pure

magnetite towards ulvospinel (Figure 9). Both Dyar et al. (2006) and Morris et al. (2006)

reported magnetite in their Mossbauer spectra. Righter et al. (2008, 2014) report trellis

type exsolution lamellae in the titanomagnetite indicating oxy-exsolution.

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Figure 8: Pyroxene and olivine chemistry in the MIL pairs, as well as some other nakhlites for

comparison (from Udry et al., 2012).

Figure 9: Compositional variation in the magnetite-ulvospinel solid solution in MIL 03346 (from

Day et al., 2006).

Glass: Feldspathic-glass compositions in the mesostasis are An29-38Or7-14 (Anand et al.

2005; Day et al. 2006).

Silica: Anand et al. (2005) and Mikouchi et al. (2005) report small (5 micron) blebs of

silica in the mesostasis. Chennaoui Aoudjehane et al. (2006) used cathodoluminescence

to study shock effects.

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Amphibole: Sautter et al. (2006, 2007) reported the presence of Cl-rich amphibole (1.5

to 7% Cl) in melt inclusions in augite and in olivine.

Phosphates: Fries et al. (2006) studied phosphates in MIL 03346 by confocal Raman

imaging techniques and found that they were “hydrated”.

Sulfides: Day et al. (2006) found that sulfide “blebs” are pyrrhotite – often altered.

Jarosite: The Martian sulfate mineral jarosite has been discovered in melt inclusions in

augite (McCubbin et al. 2008) and in the interstices of MIL 03346 (Vicenzi et al. 2007).

Saponite: Imae and Ikeda (2007) reported an occurrence of a hydrated phase (saponite?),

adjacent to fayalite, in a trapped melt inclusion – suggesting that the alteration occurred

on Mars. Hicks et al. (2013) carried out a detailed study of the saponite.

Weathering (terrestrial and martian)

Weathering on the surface of Mars has produced specific mineral assemblages, and

terrestrial weathering has also affected the MIL nakhlites with a great diversity of phases

documented and analyzed. Distinguishing between these two weathering environments is

not easy, and has been the goal of many detailed studies. Kuebler (2013) reports laihunite

that hosts stilpnomelane, as well as gypsum and bassanite, in MIL 03346 (Figure 10

middle), and argued that all phases originated on Mars. Ling and Wang (2015) made

Raman spectroscopic and Raman imaging studies of MIL 03346, with an emphasis on the

secondary mineral phases. Their study revealed three types of calcium sulfates (including

basanite and γ-CaSO4), a solid solution of (K, Na)-jarosite, and two groups of hydrated

species in the veins and/or mesostasis areas of the meteorite. They argue that bassanite

may have formed by direct precipitation from a Ca-S-H2O brine, and that the close spatial

relationship of (K, Na)-jarosite solid solutions with rasvumite (KFe2S3), magnetite, and

alkali feldspar in the mesostasis suggests in situ formation of mesostasis jarosite from

these Fe-K,Na-S-O-H2O species. Hicks et al. (2014) found amorphous olivine gel

associated with martian weathering and with saponite in some other nakhlites. Hallis et

al. (2014) found jarosite and gypsum, amorphous silicates, and Fe-oxides and hydroxides

in studies of MIL 090032. Their smectite may be the same amorphous silicate found by

Hicks et al. (2014). Cartwright et al. (2013) found noble gas and halogen evidence for

brines playing a role in surface weathering processes on Mars. Stopar et al. (2013) found

many secondary phases likely resulting from aqueous processes, including formation of

poorly crystalline iddingsite-like veins in olivine, the precipitation of Ca-, Fe-, and K-

sulfates from evaporating fluids, alteration of titanomagnetite to secondary Fe-oxides, and

the dissolution of magmatic Ca-phosphates and residual glass in the mesostasis (Figure

10, left and right). Stopar et al. (2013) emphasized that although some of the secondary

minerals may have originated on Mars, elevated S and REEs, Ce anomalies, and

association of secondary minerals with post-impact cracks and voids indicate that

terrestrial weathering has significantly affected MIL 03346. Distinguishing martian from

terrestrial weathering can be difficult and is the topic of ongoing research.

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Stopar et al. (2013) found evidence for etch-pits and olivine dissolution textures which

were also documented by Velbel (2016) and ascribed to terrestrial weathering.

Whole-rock Composition

The whole rock composition has been determined by Anand et al. (2005), Barret et al.

(2006) and Day et al. (2006) (Table 2). Barrat et al. (2006) found that Co, Ni, Cu and Zn

were like other nakhlites. The large ion lithophile elements are similar in relative

abundances to other nakhlites, but elevated, compared with Nakhla and Lafayette (Figure

11). Note the lack of any Eu anomaly. Dreibus et al. (2006) reported 147 ppm F, 248

ppm Cl, 0.45 ppm Br, 610 ppm S and 315 ppm carbon. Shirai and Ebihara (2008) have

also analyzed MIL 03346 (data reported in diagrams). Wang and Becker (2017) reported

bulk Cu and Ag data.

Figure 10: Left – jarosite (magenta) within an alteration vein from Stopar et al. (2008); Middle

–laihunite (blue) in the mesostasis of MIL 03346 from Kuebler et al., 2013); Right – Ca-sulfite

along alteration veins and zones for MIL 03346 from Stopar et al. (2008).

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Figure 11: REE diagram for MIL 03346 compared to several other nakhlites (from Day

et al., 2006).

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Table 2: Whole rock composition for MIL nakhlites

reference Anand2005

Barrat2006

Day2006

weight SiO2 % 49.2

49.5 (b)

TiO2 0.07

0.69 (a) 0.68 (b)

Al2O3 3.59

3.66 (a) 4.09 (b)

FeO 19.23

19.12 (a) 19.1 (b)

MnO 0.45

0.46 (a) 0.46 (b)

MgO 9.33

9.99 (a) 9.26 (b)

CaO 15

15.75 (a) 14.4 (b)

Na2O 1.01

1 (a) 0.96 (b)

K2O 0.29

0.27 (a) 0.2 (b)

P2O5 0.22

0.25 (a) 0.23 (b)

S %

0.06 (b)

sum

Sc ppm 46

54.5 (a) 52.9 (c )

V 184

208 (a) 210 (c )

Cr 1300

1192 (a) 1300 (c )

Co 25

35.7 (a) 38.7 (c )

Ni 60

49 (a) 58.1 (c )

Cu 13

8.2 (a) 13.3 (c )

Zn 65

61.3 (a) 61.5 (c )

Ga

6.51 (a) 6.77 (c )

Ge ppb As Se Rb

4.14 (a) 4.41 (c )

Sr 106

131.7 (a) 121.3 (c )

Y 7

8.44 (a) 8.5 (c )

Zr

23.29 (a) 21.2 (c )

Nb

3.98 (a) 3.65 (c )

Mo Ru Rh Pd ppb Ag ppb Cd ppb In ppb Sn ppb Sb ppb Te ppb Cs ppm

0.29 (a) 0.27 (c )

Ba 53

59.58 (a) 56.9 (c )

La

4.7 (a) 3.89 (c )

Ce

11.01 (a) 11.3 (c )

Pr

1.56 (a) 1.78 (c )

Nd

7.07 (a) 8.04 (c )

Sm

1.64 (a) 1.83 (c )

Eu

0.522 (a) 0.52 (c )

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Gd

1.73 (a) 1.86 (c )

Tb

0.266 (a) 0.3 (c )

Dy

1.57 (a) 1.66 (c )

Ho

0.317 (a) 0.32 (c )

Er

0.851 (a) 0.84 (c )

Tm

0.13 (c )

Yb

0.766 (a) 0.8 (c )

Lu

0.114 (a) 0.13 (c )

Hf

0.69 (a) 0.66 (c )

Ta

0.23 (a) 0.21 (c )

W ppb

0.4 (a) Re ppb

Os ppb Ir ppb Pt ppb

Au ppb Th ppm

0.42 (a) 0.43 (c )

U ppm

0.09 (a) 0.11 (c )

technique: (a) ICP, (b) e.probe (c ) ICP-MS

Radiogenic Isotopes

Murty et al. (2005) determined a U,Th-4He age of 1.02 ± 0.15 Ga and K-Ar age of 1.75 ±

0.26 Ga (based on U, Th, K contents of Nakhla). Bogard and Garrison (2006) determined

an Ar plateau age of 1.44 ± 0.02 Ga. More extensive work on MIL 03346 and its pairs

reveal Ar-Ar ages of 1.368 ± 0.083 Ga (mesostasis) and 1.334 ± 0.054 Ga (pyroxene)

(Park et al., 2009; Figure 12), and 1.373 +/- 0.011 Ga (from Cassata et al., 2010; Figure

13). A comprehensive look at nakhlites by Cohen et al. (2017) shows an age of 1.392 +/-

0.010 Ga (Figure 14) as well as variation in ages within the nakhlites that range from 1.3

to 1.4 Ga (Figure 15), with MIL among the oldest. Shih et al. (2006) determined a Rb-Sr

isochron of 1.29 ± 0.12 Ga and a Sm-Nd isochron of 1.36 ± 0.03 Ga (Figures 16 and 17).

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Figure 12: Ar-Ar age data and K/Ca data for MIL 03346 from Park et al. (2009 for whole rock

and pyroxene.

Figure 13: Ar-Ar age data and Ca/K data for MIL 03346 from Cassata et al. (2010).

Figure 14: Ar-Ar age data for MIL 03346 from Cohen et al. (2017).

Figure 15: Summary of Ar-Ar age dating by Cohen et al. (2017) for all nakhlites.

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Figure 16: Rb-Sr isochron for MIL 03346 from Shih et al. (2006).

Figure 17: Sm-Nd isochron for MIL 03346 from Shih et al. (2006).

Age data for MIL03346

Ar/Ar Rb/Sr Nd/Sm

Bogard and Garrison 2006 1.44 ± 0.02

Park et al. (2009) 1.368 ± 0.083

1.334 ± 0.054

Cassata et al. (2010) 1.373 ± 0.011

Cohen et al. (2017) 1.392 ± 0.010

Shih et al. 2006 1.29 ± 0.12

1.36 ± 0.03

Stable Isotopes

Many stable isotope studies are aimed at deciphering the building blocks of Mars, such as

Ba, Li, Ca, Si, Mg, and Fe isotopes.

MIL samples were part of a study of Ba isotopes in the inner solar system (Bermingham

et al., 2016). Ba isotope homogeneity in the early inner Solar System is evidenced by the

Ba isotope compositions of H-chondrites, enstatite chondrites, eucrites, and Martian

meteorites, which are all indistinguishable from terrestrial values.

MIL 03346 was used, along with a suite of martian meteorites, to estimate the Li isotopic

composition of the martian mantle. This work by Magna estimated the 7Li for Mars to

be 4.2 +/- 0.9, within error of the estimate for Earth’s mantle 3.5 +/- 1.0 (Magna et al.,

2015a).

Magna et al. (2015b) measured Ca isotopes in a suite of martian meteorites, including

MIL, and found that Mars has identical Ca isotopic composition to the Earth and Moon.

They suggest the inner solar system is homogeneous with respect to Ca isotopic

composition.

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Zambardi et al. (2013) measured Si isotopes in a wide range of terrestrial and achondrite

meteorites (including MIL) and found that Mars overlaps with HEDs and chondrites but

are distinctly lighter than lunar and terrestrial samples. This difference could be

explained by terrestrial core formation at high PT reduced conditions, and especially if

Moon was derived from Earth’s mantle.

Magna et al. (2017) examined Mg isotopic composition of a suite of martian meteorites

and made a similar finding to that for Li and Ca – that Mars silicate mantle has a 26Mg

value that is identical to that for the rest of the inner solar system.

Paniello et al. (2012) measured 66Zn in lunar, martian, and terrestrial samples (including

MIL) and found that martian shergottites and nakhlites essentially overlap terrestrial

mantle samples. Lunar samples on the other hand, exhibit a wide range of Zn isotopic

values suggesting potential for Zn fractionation in dry reduced magmatic environments as

well as fire fountaining.

Finally, Sossi et al. (2016) and Wang et al. (2016) measured Fe isotopes in a suite of

martian meteorites (including MIL) and found that when all are corrected for magmatic

fractionation, the martian mantle has 57Fe slightly lighter than Earth, but identical to

chondrites and HEDs. This finding is similar to that for Si isotopes.

Several studies of S, Cl, and Zn isotopes are primarily aimed at understanding magmatic

processes – see section below.

Cosmogenic Isotopes

Murty et al. (2005) determined an average exposure age of 9.5 ± 1.0 Ma for MIL 03346,

which is the number one gets for all the nakhlites.

Petrology

Mineralogic studies of the MIL augites have placed important constraints on the cooling

rates, oxygen fugacity and volatile content of the MIL parent magma.

Cooling rates

Hammer et al. (2009) examined textural features in MIL and deduced cooling rates of

~20 ˚C/hr., when compared to experimental constraints. Alvaro et al. (2015) show that

the closure temperatures of MIL augite, based on Fe-Mg ordering, are ~600 ˚C, which

correlates with a cooling rate near 6.8 ˚C/hr., slightly higher cooling rates than those

proposed by Domeneghetti et al. (2006, 2013). Studies of Li zoning and diffusion in

augite (Beck et al., 2006; Richter et al., 2014, 2016) show that MIL likely experienced

slow cooling in a magma chamber followed by relatively rapid cooling during and after

emplacement in a thin lava flow. Moreover, the cooling rates indicate that the lava flow

drained shortly after emplacement.

Oxygen fugacity

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MIL is thought to have a relatively high fO2 based on the presence of fayalite-rich olivine,

titanomagnetite and silica (Righter et al., 2008) and the Ti/Al ratio in Ca-pyroxene

phenocrysts is similar to experimental samples crystallized at fO2’s ranging between the

QFM and NNO buffers (Hammer and Rutherford 2005). Righter et al. (2008) calculated

Fe2O3 = 3.20-3.27 (XFe3+ = 0.20) in augite, which is high for martian augites. McCanta et

al. (2009) showed that Eu partitioning in augite also suggests IW+3.2 for MIL

crystallization, close to FMQ buffer. Righter et al. (2014) summarize fO2 constraints on

MIL formation and show that it may have initially crystallized near FMQ, increased

slightly during crystallization in a magma chamber, followed by reduction during sulfur

loss and degassing, and finally late oxidation due to Cl degassing and loss. This detailed

history illustrates how a single rock can contain a record of the fO2.

Figure 18: exsolution in titanomagnetite (left) and fO2 history of MIL and other nakhlites

based on summary in Righter et al. (2014).

Volatiles

McCubbin et al. (2013) show that apatites record the presence of a Cl-rich magmatic fluid

during the intermediate stages of magma emplacement. Cl-amphiboles in melt inclusions

also record the history of a Cl-rich fluid. Later degassing of Cl affects the Cl content of

the apatite, as well as the oxidation state of the magma (Righter et al., 2014). Filiberto et

al. (2016) reviews the F, Cl, and water content of the martian mantle, concluding that

martian magmas had similar water, Cl, and F contents to mid-ocean ridge basalt.

Cl isotopes were measured in MIL by Williams et al. (2016), who found that martian

meteorites in general range from 37Cl = -3.8 (mantle) to (+)ve values that are observed in

the crust. MIL falls intermediate which suggests that the nakhlites were affected by fluid

interaction or assimilation and/or fractional crystallization processes.

Franz et al. (2014) and Dottin et al. (2018) measured S isotopic values for MIL and found

that the 33S values coupled with the abundant titanomagnetite argue for assimilation of

sulfate or sulfate-bearing brines by the nakhlite parent magma. They also suggest that

MIL formed at the bottom of the nakhlite pile rather than near the top as usually argued.

Such a position might be consistent with the bulk S contents of the mesostasis as well as

other geochemical features and S degassing (Dottin et al., 2018).

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Differentiation

Wadhwa and Borg (2006) found that the 142Nd and 182W isotopic anomalies were like

other nakhlites, concluding that nakhlites formed under relatively oxidizing conditions.

Debaille et al. (2007, 2008) found evidence from the time integrated isotopic evolution of

Sm-Nd and Lu-Hf system for early differentiation of the martian mantle, perhaps

reflecting deep mantle phases and thus deep mantle fractionation in the early history of

Mars. The 142Nd-143Nd record of the nakhlites is difficult to interpret because the

nakhlites plot outside the two-stage evolutionary field in the 142Nd vs. 143Nd diagram

defined by shergottites (Debaille et al., 2009). The 146Sm-142Nd systematics of the

nakhlites are like those of the depleted shergottites, whereas the 147Sm-143Nd systematics

reveal differences, which may indicate a disturbance of the Sm-Nd system after extinction

of 146Sm. Although the 146,147Sm-142,143Nd systematics of the SNC meteorites exhibit

evidence for differentiation of the Martian mantle 10-100 Ma after solar system

formation, exact scenarios are model dependent and remain under investigation.

Figure 19: Nd-W isotopic diagram showing values for the nakhlites (open square) that is

like depleted shergottites but lies at a higher W value (from Debaille et al., 2009).

Miscellaneous studies

Blamey et al. (2015) measured methane and hydrogen released from MIL olivine and

pyroxene, concluding that these gases were trapped in fluid inclusions or along fractures,

and demonstrate that the martian subsurface is capable of hosting microbial life.

Murty et al. (2005) reported the isotopic ratios of rare gases extracted at different

temperatures from MIL 03346.

Dyar et al. (2006) determined the Mossbauer, reflectance and thermal emission spectra of

MIL 03346 (Figures 20, 21), arguing that this rock is highly oxidized with abundant Fe3+.

Kanner et al. (2007) studied spectroscopy of MIL 03346 and integrated the result into

comprehensive examination of low and high Ca pyroxene modelling with OMEGA data.

Coulson et al. (2007) measured porosity (2.97 to 3.60 %) for MIL 03346.

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Gattacecca et al. (2005) and Jambon et al. (2010) reported the magnetization of MIL

03346 and show that the intensity fabric is oblate, not unlike many terrestrial plutonic and

volcanic rocks.

Figure 20: Mossbauer spectra of MIL 03345 whole rock and clinopyroxene separate

(from Dyar et al., 2006).

Figure 21: Reflectance spectra of MIL 03346 and Nakhla (from Dyar et al., 2006).

Summary

MIL 03346 and its pairs have obviously contributed to our understanding of the geology

of Mars - from the chemical building blocks of Mars to the timing and conditions of its

early differentiation, to mantle melting, magma genesis and magmatism (volatiles and

cooling history), to more recent weathering and surface processes. It has provided

information about the magnetic field of Mars, organic geochemistry, and surface

spectroscopy, and in general the redox evolution of Mars and its magmatic rocks. These

samples will undoubtedly continue to provide important constraints on the geochemical

and geophysical evolution of Mars.

Processing

NASA-JSC received more than 50 requests for this sample for the Fall 2004 Meteorite

Working Group meeting. As of 2014, it had been subdivided into >200 splits and

distributed to ~70 scientists around the world for study. Righter and McBride (2011),

Allen et al. (2011), and Righter et al. (2014) have presented information about the

processing and allocation of MIL 03346. MIL 03346 was examined and split in dry-

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nitrogen glove boxes at JSC which have been thoroughly cleaned and dried immediately

before processing of this sample. The sample was only exposed to stainless steel,

aluminum and Teflon, although the gloves, gaskets and band saw wheels are made of

Neoprene and/or Viton. However, the sample itself was only handled with Teflon

overgloves.

MIL 03346 was subdivided in three main stages: initial processing (13.15 g including 5

thin sections), slab allocations (46.46 g including 49 chips and 7 thin sections), and NE

butt end allocations (32.05 g including 8 chips and 1 thin section butt). Small pieces were

derived for the initial characterization of the sample, including a 2.1-g chip that was

potted to make thin sections (Figure 22 and 23). Due to the large number of individual

samples requested, bandsaw slabbing was considered the best way to preserve as much of

the original mass as possible for future study while also documenting individual meteorite

chips allocated (Figure 24-25). After the slab was totally subdivided and allocated (Figure

25), the NE butt end was subdivided (Figure 26). The total allocated mass of the main

mass, the slab, and the NE butt end are summarized in Table 3.

After nearly 14 years of curation and study, much has been learned about Mars for the

MIL pairing group, as summarized above. A 447-g piece of the main mass of MIL 03346

remains for future studies, as well as a total of ~600 g of material that has not been

allocated. Clearly, many additional future studies are possible with this much mass

available.

Table 3: Summary of major subdivisions of MIL 03346 (as of 2014)

Figure 22: Subdivision history of MIL 03346, circa 2005.

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Figure 23: Summary of initial processing of MIL 03346.

Figure 24: Derivation of slab of MIL 03346 by bandsawing.

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Figure 25: Subdivision of the MIL 03346 slab

Figure 26: Subdivision of the NE butt end (SW view).

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References for MIL03346, 090030, 090032, 090136 (compiled by C. Meyer, Oct 2012; updated by K. Righter Oct. 2018)

Allen, C., Allton, J., Lofgren, G., Righter, K., Zolensky, M. E. (2011) Curating NASA's

extraterrestrial samples-Past, present, and future, Chemie der Erde - Geochemistry 71, 1-20,

http://dx.doi.org/10.1016/j.chemer.2010.12.003.

Alvaro, M., Domeneghetti, M. C., Fioretti, A. M., Camara, F., Marinangeli, L. (2015) A new

calibration to determine the closure temperatures of Fe-Mg ordering in augite from

nakhlites, Meteoritics & Planetary Science 50, 499-507.

Anand M., Williams C.T., Russell S.S., Jones G., James S., and Grady Monica M. (2005a)

Petrology and geochemistry of Nakhlite MIL03346: A new martian meteorite from

Antarctica (abs#1639). Lunar Planet. Sci. XXXVI Lunar Planetary Institute, Houston.

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characteristics of Nakhlite MIL03346: Records of crustal processes on Mars (abs#5257).

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