MURCHISON

On a Sunday morning at 10:58 a bright orange fireball exploded with loud detonations and hissing noises. Hundreds of stones rained down over Victoria, Australia covering 5 square miles, permeating the town with the odor of alcohol. Over 700 charcoal-colored stones with a total weight of over 100 kg were collected, the largest mass weighing 7 kg.

Murchison is a breccia that contains mm- to cm-sized xenoliths of mostly type-3 carbonaceous chondrite provenance. Murchison has a shock stage of S1–2 and a weathering grade of W1–2. The CM chondrites have undergone extensive aqueous alteration on the parent body, the degree of which having been determined by such factors as water/rock ratio, temperature, and duration of the process. An early alteration sequence for CM chondrites was proposed by Ikeda (1983), by which most Murchison chondrules would be designated stage-II:

Utilizing petrography and mineralogy, Browning et al. (1996) observed several features correlated to an increase in hydration, among which was a progression from Fe-rich serpentine to Mg-rich serpentine. Based on these indicators they arranged a set of CM chondrite falls in a sequence of increasing relative aqueous alteration as follows:

Murchison ≤ Bells < Pollen ≤ Murray < Nogoya < Mighei < Cold Bokkeveld

Results of a petrological, geochemical, and reflectance spectral study (diversity in the 3 µm band center) involving a set of CM chondrites, conducted under dry and vacuum conditions, has led Takir et al. (2013) to establish three spectral groups corresponding to an increasing state of hydration, and which could be applied to the interpretation of spectroscopic observations of asteroids:

• Group 1 (least aqueously altered) phyllosilicates composed of Fe-serpentine (cronstedtite) corresponding to subtypes 2.6–2.3
• Group 2 (intermediate aqueous alteration with intermediate mineralogical phases)
• Group 3 (most aqueously altered) phyllosilicates composed of Mg-serpentine (antigorite) corresponding to subtypes 2.2–2.1

Building upon and strengthening the basis for a unique scale reflecting the degree of aqueous alteration, Rubin et al. (2005, 2007) proposed a new alteration sequence for CM chondrites. Based on eight major diagnostic parameters of progressive alteration, they classified Murchison as a petrologic type 2.5, which, along with the other CM chondrites, was derived from a hypothetical precursor lithology having a petrologic type 3.0, broadly similar to the anhydrous, ungrouped (probably CO-related; Simon and Grossman, 2015), type-3.0 Acfer 094, or perhaps the CO3.0 ALHA77307. Following are the major parameters developed by Rubin et al. (2007) for estimating the degree of alteration of the CM chondrites:

early to intermediate stage alteration processes:

1. hydration of fine-grained matrices to form phyllosilicates, which gradually consists of Mg-rich serpentines
2. conversion of primary chondrule glass to phyllosilicate
3. production of large PCP (tochilinite–cronstedtite intergrowths [TCI]) clumps

processes occurring throughout the alteration sequence:

4. oxidation of FeNi-metal
5. alteration of chondrule silicate phenocrysts
6. compositional and size changes of TCI (e.g., depletion in S and "FeO" [FeO in phyllosilicates, Fe⁺³ in cronstedtite, and Fe⁺² in sulfide]; SiO2, TiO2, Cr2O3, MnO, and CaO enrichment; decrease in size)
7. formation of increasingly complex carbonates (e.g., calcite => dolomite)
8. compositional changes in sulfides

In a study by Kimura et al. (2020) of the least altered (both aqueous and heat) CM chondrites Asuka 12085, 12169, and 12236, they extended the diagnostic characteristics presented by Rubin et al. (2015) for CM petrologic subtypes 2.7–2.0 to further distinguish subtypes 3.0–2.8 (see their chart here). Kimura et al. (2020) also concluded that despite the very close mineralogical and O-isotopic compositions, CM and CO chondrites most likely formed on separate parent bodies.

Howard et al. (2015) established an aqueous alteration scale for the CM chondrites (as well as CR and C2-ungrouped chondrites) based on the phyllosilicate fraction (total phyllosilicate/total anhydrous silicate + total phyllosilicate). Through modal measurements utilizing Position Sensitive Detector X-ray Diffraction (PSD-XRD), and defining the sub-types in increments of 5% of the abundance of phyllosilicate, they found that CM chondrites fall in the range of 1.7–1.2 in their classification scheme (see endmember example below). However, King et al. (2015) reasoned that because alteration might continue even after all silicates have been hydrated, this scheme could be difficult to extend to CI chondrites in which members reflect similar phyllosilicate abundances but show variable degrees of alteration in other features. Moreover, unlike the Howard scale, the petrologic subtype classification of Rubin et al. (2005) takes into account compositional variation in phyllosilicates and tochilinite that occurs with increasing alteration (OH/H₂O band variation), which provides a higher comparative resolution across the CM suite (Hanna et al., 2020).

Both the CM chondrite petrologic subtype classification of Rubin et al. (2005) and the CR chondrite petrologic subtype classification of Harju et al. (2015) can be converted to the alteration scale of Howard et al. (2015) using the following equation:

In their study, de Leuw et al. (2009, 2010) found that CM chondrites which have lower petrographic subtypes experienced longer durations of aqueous alteration. Analyzing carbonates in CM chondrites, they determined that correlations in the Mn–Cr systematics were indicative of in situ decay of 53Mn during carbonate formation. They were able to utilize the correlation between the degree of aqueous alteration and the age of carbonate formation to arrive at a duration for such alteration of at least 4 m.y. It was shown that the carbonates that are the least altered are the oldest and vice versa. It was also concluded that FeCO3 can be used as a taxonomic parameter. The least-altered CM chondrites (petrologic type ≥2.4) have more abundant FeCO3 contents than those that are more-altered (petrologic type ≤2.4). Table A below shows the features present in the FeNi-metal and sulfides in CM and CY chondrites that are associated with the heating stage (Nakamura, 2005; Kimura et al., 2009), while Table B below shows the heat-related changes observed by XRD patterns associated with each heating stage (King et al.. 2021).

Kimura et al. (2011) revised this classification scheme by assigning a heating stage category A–C to CM chondrites. Category A (unheated) corresponds to heating stage I above. Category B (300°C to 750°C) corresponds to heating stage II and III above. Category C (>500°C to >750°C) corresponds to heating stage III and IV above. The presence of primordial metal in the form of martensite attests to a low degree of secondary thermal alteration following aqueous alteration in the case of Murchison. The placement of Murchison in Category A is a reflection of the metal composition (Ni content) and the sulfide texture (abundance of pentlandite blebs in pyrrhotite) of this meteorite.

Hanna et al. (2020) obtained IR reflectance spectra from thin sections for a suite of CM chondrites and found that certain spectral trends in the wavenumber region <1200 cm^–1 were correlated with the petrologic subtype: the separation (wavenumber distance) between the Christiansen Feature (CF) and the Si-O stretching band minimum was highly correlated (R² = 0.90) with the petrologic subtype to an accuracy of 0.1 (see diagram below), while other spectral parameters such as Mg-OH band depth, CF position, and Si-O bending minimum were correlated to a lesser degree (R² = 0.87, 0.82, and 0.82, respectively). In particular, as aqueous alteration increases (i.e., lower petrologic subtype), the CF (~1100 cm^–1) shifts to lower wavenumbers, the Si-O stretching (~950 cm^–1) and Si-O bending (~440 cm^–1) band minima shift to higher wavenumbers, the separation of the CF and Si-O stretching band minimum decreases, and the depth of the Mg-OH band (~625 cm^–1) increases. Hanna et al. (2020) ascertained that the spectral trends observed in the wavenumber region <1200 cm^–1 reflect the proportionate change of primary anhydrous silicates to secondary phyllosilicates corresponding to increasing aqueous alteration.

Murchison contains sparse chondrules with diameters between 0.1 mm and 0.5 mm, composed of individual phenocrysts of olivine and pyroxene. Porphyritic chondrules contain some FeNi-metal grains. The chondrule mesostasis has been altered to phyllosilicates—Fe- and Mg-serpentines. The black matrix constitutes ~48 vol% of the meteorite and is similar to that of the CI matrix, but contains less magnetite. Chondrule fragments and olivine crystals are abundant in the Murchison matrix, while the CAI content is low. Isotopic research indicates that the matrix and chondrules of pristine carbonaceous chondrites probably condensed during the same heating event (Nyquist et al., 2009). Carbonate grains that formed in situ under low temperature conditions of 0–25°C are present in amounts of a few vol%, which consist predominantly of calcite/aragonite with minor amounts of dolomite, along with low abundances of sulfides.

Interestingly, newly identified refractory inclusions in Murchison composed primarily of hibonite represent some of the earliest condensed solids or residues from the early, hot, solar nebula (Liu et al., 2009). These refractory grains comprise platy crystals (PLACs), spinel–hibonite spherules (SHIBs), and blue aggregates (BAGs). PLACs lack resolvable 26Mg-excesses (the daughter product of 26Al [see full description]) and were formed within a timespan of ~100,000 years in an 16O-enriched, heterogeneous region (based on anomalous δ48Ca and δ50Ti isotopic signatures) prior to incorporation and mixing of short-lived nuclides such as 26Al into the solar nebula through injection of interstellar dust. Both PLAC and BAG formation occurred hundreds of thousands of years prior to the formation of CV CAIs. In contrast, SHIBs formed later by condensation of precursor material in a lower temperature environment than that of PLACs. They record in situ 26Al decay and "canonical" initial levels of 26Al/27Al, and they are considered to have formed 100,000–300,000 years after the formation of CV CAIs. Some hibonite grains in Murchison have experienced Rayleigh fractionation through distillation/evaporation, while some also exhibit nuclear anomalies showing similarities to the FUN group of CAIs studied in CV3 Allende.

X-ray diffraction techniques and Mössbauer spectroscopy have been used by Bland et al. (2004) to determine the modal mineralogy of several carbonaceous chondrites including Murchison. They were also able to quantify the compositional range of the olivine phases. In addition, the grain density can be readily estimated from the mode data, and therefore, in combination with the calculated bulk density, the porosity can be determined. The modal mineralogy (vol%) and other physical properties of Murchison were determined to be as follows:

• Olivine
• Fo100 -------------------- 6.8
• Fo80 --------------------- 1.9
• Fo50 --------------------- 1.6
• Clinoenstatite (En98) --------- 1.9
• Pyrrhotite ---------------------- 1.8
• Pentlandite --------------------- 0.3
• Magnetite ----------------------- 0.2
• Serpentine --------------------- 26.2
• Calcite --------------------------- 1.2
• Tochilinite/Cronstedtite ---- 58.1
• TOTAL ----------------------- 100.0
• grain density = 2.92 g/cm³
• bulk density = 2.20 g/cm³
• porosity = 24.7 vol%

A more technologically advanced determination of the Murchison modal (vol%) mineralogy was conducted by Howard et al. (2009) with results as follows:

• Olivine ---------------------------15.0
• Clinoenstatite (En98) ---------- 8.3
• Pyrrhotite ----------------------- 1.2
• Pentlandite --------------------- 0.65
• Magnetite ----------------------- 1.1
• Serpentine --------------------- 22.0
• Calcite --------------------------- 1.2
• Cronstedtite ------------------ 50.0
• TOTAL ------------------------ 99.45

Dark, fine-grained (<1 µm) material (DFM) which forms opaque mantles surrounding chondrules, refractory inclusions, and matrix silicates, are believed by some to be accretionary features from solar nebula dust reservoirs unrelated to the silicate cores on which they are found. An investigation by Trigo-Rodriguez et al. (2006) of the variable porosities within these dark rims indicated that they were formed on the parent body through impact-compaction of fine-grained, porous matrix material, followed by aqueous alteration and the deposition within the mantle of what was historically termed "poorly characterized phases" (PCP). This phase has now been determined to be tochilinite–cronstedtite intergrowths (TCI). The TCI are present in two distinct forms as described by Pignatelli et al. (2016) in the least altered CM chondrite Paris:

1. type-I: rounded- or irregular-shaped secondary alteration phase composed primarily of sulfur-rich tochilinite with lesser abundance of cronstedtite and magnetite; usually observed as zoned rims around precursor FeNi-metal beads within chondrules, in which cronstedtite increases in proportion to tochilinite progressing outwards from the rim.
2. type-II: round-, anhedral-, or euhedral-shaped secondary alteration phase located within the matrix, constituting two concentric zones of variable thickness; the outer zone is composed of variable proportions of tochilinite and cronstedtite, while the inner zone is composed of a porous, fibrous-textured, Fe-hydroxide mineral amakinite.

Type-I TCI formed when precursor kamacite particles reacted with ionized, S-bearing, alkaline water at low temperatures of ~50–100°C under reducing conditions involving a stable temperature and pressure (Peng et al., 2007). Type-II TCI formed as a complex secondary alteration phase by a step-wise dissolution/reprecipitation process through interaction with an evolving fluid (high-S ⇒ low-S + high-Si ⇒ low-S + low-Si), ultimately replacing olivine, and to a lesser extent, pyroxene grains, in a localized and/or transient, micro-scale aqueous environment (Pignatelli et al., 2016).

Unlike the results of previous studies, it was demonstrated that the DFM is not confined to rims around discrete objects, but instead, can form indistinct boundaries blending seamlessly from the objects into the matrix. Moreover, the dark, fine-grained material can be found extending beyond its associated object, comprising isolated patches within matrix space, forming single rims around multiple objects, and surrounding post-aqueous alteration phases. Many smaller discrete objects have no mantles at all, inconsistent with a common nebular origin. Where DFM composes mantles around discrete objects, it forms a layered structure in which the lowest porosities adjacent to the enclosed objects reflect a high degree of compaction. Because agglomeration modeling shows that such a high degree of compaction is not attainable through nebular processes, the investigators argue that this provides supporting evidence for a parent body origin for DFM mantling through multiple impact-compaction events.

Notably, a microfabric consisting of foliations in some dark inclusions, as well as the preferred orientation of chondrules and matrix phyllosilicates, is likely the result of impact-induced deformation (Lindgren et al., 2012). In a study of deformed chondrules in Murchison using X-ray computed tomography, Hanna et al. (2014) observed both foliation (planar alignment) and lineation (much longer in one dimension than in the other two) fabrics produced by impact stress. Utilizing a combination of high-resolution X-ray computed tomography and 3-D software to study fine-grained rims on CM chondrules, Hanna and Ketcham (2015) found that a significant positive correlation exists between rim thickness and the size of the enclosed chondrule; this result supports the theory that the rims accreted in the solar nebula rather than formation through parent body processes. Similarly, Mouti et al. (2021) found no correlation between either the size or the abundance of fine-grained rims and the degree of aqueous alteration or heating, demonstrating that rim formation in CM chondrites most likely occurred in the nebula prior to parent body accretion.

Following the agglomeration and impact-induced compaction of the various components in Murchison, the material experienced high degrees of aqueous alteration at temperatures of 20–35°C within a zone ~100–250 m thick at a depth of 1–1.8 km (Guo and Eiler, 2007; Hanna et al., 2014). Studies of CM chondrite REE patterns indicate the water had a pH of 6–8 during the alteration process (Inoue et al., 2009). Low-temperature reactions involving thin fluid films promoted precipitation–dissolution processes in which Fe- and S-bearing phyllosilicates replaced host minerals. Nanotubes have been identified in both Murchison and Mighei (Zega et al., 2004) which are believed to have condensed from low-temperature, S-rich, aqueous solutions. They are composed of a new serpentine phase intermediate between cronstedtite and chrysotile. It was found by Rubin (2012) that the CM chondrites composed of higher-porosity material were affected by higher degrees of shock deformation and fracturing and exhibit stronger petrofabrics, features which facilitated a subsequent commensurate higher degree of aqueous alteration, i.e., lower petrologic subtype. Contrariwise, probably due to their lower porosities, lower matrix abundances, and less bulk water content, the CR-group chondrites do not exhibit a similar correlation between shock features and degree of aqueous alteration (Rubin and Harju, 2012).

As shown above, Rubin et al. (2007) consider Murchison to be one of the least altered CM chondrites, and it can be placed within an aqueous alteration sequence with other CM members from most to least aqueously altered as follows: MET 01070 [2.0], QUE 93005 [2.1], Cold Bokkeveld [2.2], QUE 99355 [2.3], Y-791198 [2.4], Murray [2.4/2.5], Murchison [2.5], and QUE 97990 [2.6]. However, Bischoff et al. (2017) and Lentfort et al. (2019) recognized that most CM chondrites are breccias that exhibit variable degrees of alteration among the different clasts (or among different "poorly characterized phases" [PCP]) within a given meteorite. Therefore, they propose a more precise classification scheme that reflects this range of alteration subtypes, and suggest new subclassifications for a number of CM chondrite breccias based on geochemical analyses of TCIs in individual fragments (*using only "FeO"/SiO2 ratios in Lentfort et al., 2020) as follows:

"FeO"/SiO2 THRESHOLD VALUES FOR SUBTYPES Lentfort et al. (2020)
2.0	2.1	2.2	2.3	2.4	2.5	2.6	2.7	2.8	2.9
<0.9	>0.9	>1.2	>1.6	>1.8	>2.0	>2.7	>3.3	>4.1	>4.9

*ALHA77306: CM2.0–2.6
*ALH 85013: CM2.2–2.7
*Banten: CM2.6–2.9
*Cold Bokkeveld: CM2.1–2.7
*EET 87513 (clast in HOW): CM2.6
*Jbilet Winselwan: CM2.4–2.9 (host CM2.5)
*LON 94101: CM2.0–2.8 (CM1 and CM3 clasts)
*Maribo: CM2.6 (bulk rock)
*Murchison: CM2.5–2.9 (CM6 clast; host CM2.7)
*Nogoya: CM2.2–2.5
*NWA 7542 (clasts in EUC-pm): CM2.2–2.8
*NWA 12651: CM2.7–2.8
*Santa Cruz: CM2.7 (bulk rock)
*Y-791198: CM2.4 (CM2.8 clast)

The CM chondrite Paris is a newly discovered representative reflecting a lower degree of aqueous alteration and mild thermal metamorphism. It contains an abundance of well-preserved metal with little magnetite, and has large unaltered zones and less matrix component than other CM members (Zanda et al., 2010). While initially having a CI-like composition, the matrix of CM chondrites reflects a S/Si ratio that decreases as aqueous alteration increases. This pattern demonstrates an independent accretion within diverse regions of the protosolar disk and a subsequent exchange between two components—a high-temperature fraction and a CI-like fraction—rather than accept the pre-accretion complementarity model involving these two components (Zanda et al., 2011). Other recent studies have addressed the chondrule–matrix complementarity issue and have concluded that advocacy for such a genetic relationship is unnecessary to explain the elemental ratios observed in these two components (e.g., Patzer et al., 2020). Such complementarity between chondrules and matrix can be explained by their rapid accretion from single reservoirs located at different heliocentric distances—the "single reservoir" theory invoked by Ebel et al. (2023 #6027).

The unaltered precursor material of the CM group is considered to be type CM3.0. Although Paris does contain some phyllosilicates most of its features, such as a high content of FeS in PCPs and a high chromium oxide content, indicate a tentative petrologic assignment for hydrothermal alteration of type 2.7/2.8, and a petrologic assignment for thermal metamorphism of A/B (Blanchard et al., 2011). A new investigation of Paris by Rubin (2015) revealed that some regions are even less altered and should be classified as type 2.9. This assignment is similar to that of the ungrouped (probably CO-related; Simon and Grossman, 2015) Acfer 094 and the CO3.0 chondrite ALHA77307. Paris exhibits many intermediate characteristics to the CO chondrite group (Bourot-Denise et al, 2010). Interestingly, Paris shows signs of pre-terrestrial magnetism, possibly internally generated, attesting to a former convecting metallic core (Cournede et al., 2011).

Based on advanced analytical techniques in which the modal mineralogy of a suite of CM chondrites (Mighei, Nogoya, Murchison, Murray, and Cold Bokkeveld) was quantified to a high degree of accuracy, Howard et al. (2009) more accurately resolved the degree of aqueous alteration experienced by these CM chondrites based on their total phyllosilicate abundances, measuring Mg-serpentine + Fe-serpentine (cronstedtite); Fe-rich serpentine transitions to Mg-rich serpentine as aqueous alteration progresses. The investigators found that a narrow range exists in the modal abundances of most CM chondrites with regard to phyllosilicates, anhydrous silicates, and other phases. They showed that the inverse relationship that exists between the anhydrous silicates and the phyllosilicates is reliable evidence that the latter formed from the former through aqueous alteration processes. Moreover, an inverse relationship in the abundances of Mg-serpentine and Fe-serpentine (cronstedtite) also supports an aqueous alteration process, as cronstedtite loses Fe and recrystallizes to form Mg-serpentine in the presence of water.

At the same time, since this alteration process is controlled by variable abundances of anhydrous silicates within different CM samples, the initial composition of each CM chondrite may have been variable, rendering it impossible to determine the actual extent of aqueous alteration by this method. In light of the fact that accurate measurements of phyllosilicate abundances among the CM samples have now been obtained by Howard et al. (2009), and that these abundances have been ascertained to be the same within a small range (73–79%), it may be inferred that each CM chondrite has experienced an equal degree of aqueous alteration, and the subtypes proposed by Rubin et al. (2007) (as shown above) are not accurately defined. As a result, the team argues that it is not necessary to resolve the subtype of the CM group further than CM2.

Be that as it may, Howard and Alexander (2013) have proceeded to establish an aqueous alteration classification scale (hydration scale) distinct from the thermal metamorphic classification scale, one that is based on the total abundance of phyllosilicates in a meteorite and that does not imply an evolutionary progression from lower to higher degrees of aqueous alteration. In their scheme, phyllosilicate abundance increases along the type sequence: 3.0 (0%) ⇒ 2.0 (50%) ⇒ 1.0 (100%), where the phyllosilicate abundance increases in 0.1 (5%) increments. This method allows for a consistent scale to be applied across all carbonaceous chondrite groups. A hydration indexed chart of 40 carbonaceous chondrites, comprising CI, CM, and CR group members resolved by phyllosilicate abundance, was published in an abstract by Howard and Alexander (2013), while the classifications of 54 meteorites was published in an article by Alexander et al. titled 'The classification of CM and CR chondrites using bulk H, C and N abundances and isotopic compositions', GCA, vol. 123 (2013), which was followed by an article by Howard et al. titled 'Classification of hydrous meteorites (CR, CM and C2 ungrouped) by phyllosilicate fraction: PSD-XRD modal mineralogy and planetesimal environments', GCA, vol. 149 (2015).

In further studies of hydrous alteration in carbonaceous chondrite groups, Howard et al. (2013) determined that neither the relative abundances of Fe- and Mg-rich serpentines nor the bulk O-isotopic compositions show any correlation to the degree of aqueous alteration. The investigators suggest that the Fe:Mg ratios in serpentines, as well as the final bulk O-isotopic compositions, were controlled instead by factors related to the anhydrous precursor material, e.g., the initial chondrule:matrix ratio, where the matrix is intrinsically more Fe-rich. Another controlling factor they invoke is the temporal abundance of water ice.

Murchison contains water-bearing minerals including serpentines. These phyllosilicates provide a high water content of 4–18 wt%, water that initially condensed at a distance of 4 AU from the Sun (Eiler and Kitchen, 2004). A total of 2.8 wt% of this water is adsorbed or trapped inside pores (Yoldi-Martinez et al., 2011). In Murchison, Mg-rich serpentines as well as Fe-rich cronstedite are found to contain –OH. Fe-rich aureoles are among the products resulting from in situ aqueous alteration processes. Additionally, Murchison contains carbon (2–2.5 wt%) and nitrogen (0.09–0.16 wt%) as constituents of free organic matter, diamond, and soluble complex macromolecular organic compounds (10–15 ring polycyclic aromatic hydrocarbons [PAHs]), including at least 80 amino acids (~14,000 ppb for C2–C5) and the bases that make up the biological coding elements of RNA and DNA. All of these organic compounds have a nonbiogenic origin, and were formed by such processes as irradiation of interstellar organic ices by cosmic rays. A listing of amino acids identified in Murchison before 1991 can be found on the Murchison organics page.

Further studies at the University of Bremen in Germany have led to the identification of seven diamino acids, which are the building blocks of peptide nucleic acids considered to have preceded RNA and DNA in the genesis of life. Also having an abiotic origin, a suite of over fifty monocarboxylic acids have been identified in Murchison (Huang et al., 2004), some of which have also been found in the C2 ungrouped chondrites Tagish Lake (Herd, University of Alberta, 2009) and EET 96029, the latter containing a high abundance of formic acid. Studies of Murchison at the University of California at Davis (D. Deamer) have revealed the existence of lipid-like organic chemicals able to self-assemble into a membrane-like film enclosing a fluid, an analog to a cell membrane. Although CM chondrites with lower petrologic types (extensive aqueous alteration) contain significantly less abundant amino acids compared to those with higher petrologic types, the finding of similar relative abundances among them suggests that a common parent body link may exist (Botta et al, 2007).

The case has been made, based on O-isotopic compositions, for the pre-terrestrial production of water-soluble sulfate by the oxidation of sulfides in the presence of water (Airieau, et al., 2005). This process occurred as fluid flowed through unaltered rock that still preserved a component of its original oxygen ratio. This sulfate is isotopically stable, and preserves the oxygen isotopic signature of the water that was present at the time of sulfate formation, and to some degree may also reflect the signature of the water that was present during aqueous alteration processes of the meteorite.

The isotopic composition of Murchison and other CM chondrites reflects contributions from two primary reservoirs: 1) an anhydrous silicate component similar to the primitive CO3.0 chondrite ALHA77307, and 2) an aqueous component manifest as phyllosilicates formed through parent body processes (Clayton and Mayeda, 1999). A parent body origin for the phyllosilicates is revealed by the heavy carbon (13C) content of the carbonates, which is heavier than nebular C gas. Rather than a mass fractionation process, the heavy C could have been derived from presolar carbide grains, or as proposed by Guo and Eiler (2007), through the production and escape of 13C-depleted methane during aqueous alteration. A low water/rock ratio employing isotopically-heavy water at temperatures near 0°C is considered the most likely parent body alteration environment. See the Colony page for information regarding a possible common parental source object for the CM and CO groups.

Of possible historic significance is the recent discovery of a variety of sugar compounds, collectively known as polyols, within Murchison and the similar CM2 Murray. These compounds are constituents of RNA and DNA, and serve a role in cellular chemistry. Equally remarkable, fatty acids have been isolated from Murchison that independently form boundary membranes in alkaline conditions creating a rudimentary cell structure which could theoretically lead to self-replication. Two of the known nucleobases, which when associated with a sugar and a phosphate group constitute the nucleic acids that compose the genetic code, have been identified as indigenous components in Murchison (Martinsa et al, 2009): the one-ring pyrimidine, uracil, is present as a natural component of RNA, while the two-ring purine, xanthine, is instrumental in the synthesis of other purine nucleotides.

Besides these discoveries, isotopic studies suggest that organic sulfur compounds within Murchison may have been created by interaction of carbon-disulfide molecules with light in the low-temperature, pre-planetary environment of interstellar space. Similarly, it was found that UV photolysis of interstellar ice could lead to the formation of the amino acids glycine, alanine, and serine, and could explain the existence of an L-enantiomer bias. In light of the fact that these naturally synthesized ingredients necessary for life are present in asteroidal material, the question arises: what influence did meteorite accumulation on Earth have on the genesis of terrestrial life? Interestingly, an ultrahigh-resolution analysis of the extraterrestrial organic matter in Murchison has revealed that its indigenous chemical diversity encompasses tens of thousands to millions of different molecular compositions, exhibiting a chemical complexity that is high compared to biological systems on Earth (Schmitt-Kopplin, 2010).

Murchison also contains insoluble organic compounds. One component (20%) consists of presolar diamonds in concentrations of 1000 ppm, while another (10%) consists of grains of presolar graphite and SiC. Croat et al. (2008) discovered that the graphite in Murchison is present as both ordered (onion types) and disordered (platy types and scaly types) morphologies. Some platy graphite grains contain internal refractory grains of oxides (e.g., eskolaite and magnetite), carbides, and RuFe-metal, similar to constituents found in onion type graphites. These platy grains also show enrichments in 12C. The combined isotopic and compositional evidence indicates that both the onion and platy graphite grains formed during s-process nucleosynthesis (in which neutrons are slowly added to nuclei over thousands of years) in one or more AGB carbon stars. It was further determined by the research team that the most disordered grain type, the scaly graphite, has O-isotopic ratios and other features more consistent with having originated during r-process (rapid neutron capture) nucleosynthesis occurring in supernovae.

Nguyen et al. (2007) ascertained that the SiC grains in Murchison are comprised of a predominant mainstream type (i.e., low-mass 1.5–4 M_⊙ C-rich AGB stars), plus the rare types A + B (from J-type carbon stars), X (from type II supernovae), and Y + Z (from low-metallicity AGB stars, where metallicity is based on the proportion of elements heavier than helium). The CRE ages of some large SiC grains range up to 1.5 b.y. The largest insoluble organic component (~70%) is a kerogen-like material (Mao, 2005). These components were mostly produced during s-process nucleosynthesis in aging, medium-sized carbon stars (TP-AGB phase), or very rarely in supernovae. TiC crystals thought to have been produced in supernovae, and rutile grains of variable composition thought to have been produced in AGB star outflows (Croat, 2007), along with rare SiC grains of uncertain origin (Hynes and Croat, 2007) have become internal constituents of later formed graphite grains. While one SiC grain has been determined to be from a nova, the origin of another anomalous grain highly enriched in 30Si has yet to be established. Additionally, it was discovered that the isotopic composition of some X-Type SiC grains is enhanced in heavy elements, which has given rise to the new formation theory of neutron burst nucleosynthesis. All of these interstellar grains, including aluminum oxide, spinel, and silicon nitride are remnants of the dust cloud from which our Solar System was formed.

The CM chondrites may be linked by spectral properties to the C-type, G-class asteroids 19 Fortuna and 13 Egeria, both of which are located near resonances that should be supplying fragments to Earth. On the other hand, Rubin and Bottke (2007) argue that the prevalence of CM xenolithic clasts in ordinary chondrites and HED breccias is consistent with a recent collisional fragmentation event. They believe the source to be an ~170-km C-type asteroid located in the inner asteroid belt that had been disrupted ~160 m.y. ago, and which now comprises the Baptistina asteroid family. The close proximity of this asteroid family to the ν₆ resonance, as well as the similar orbits of the OC and HED parent bodies, support such a scenario. Nonetheless, contradictory spectroscopic data have been obtained by Reddy et al. (2009), including analysis of absorption features and albedo values, suggesting that 298 Baptistina is more consistent with an S-type asteroid, perhaps similar to the LL chondrites, and is inconsistent with a carbonaceous chondrite. In a spectroscopic analysis of the CM2 chondrite Mukunpura, Izawa et al. (2019) demonstrated that a close match exists to the near-Earth asteroid NEA 1999 JV6 in the near-IR wavelengths (see diagram below). They infer that NEAs such as this could be the parent body(ies) of some CM2 meteorites.

Interestingly, the recorded fall of the CM chondrite Maribo may provide a link to Comet Encke within the Taurid complex. The very high eccentricity derived for the pre-atmospheric orbit of Maribo, as well as the location of the semimajor axis within the main asteroid belt, are nearly identical to those of Comet Encke (Haack et al., 2011). In addition, significant similarities exist in the D/H ratio between the water present in certain comets, such as Halley and Hyakutake, and that observed in carbonates and phyllosilicates present in CM chondrites. Similarities also exist in the mineralogy of CM chondrites and the samples returned from Comet Wild 2, while high annealing temperatures are required in both to produce their crystalline silicate component. However, a large disparity in CRE ages exists between CM chondrites and that conjectured for the Taurid complex comets—the Murchison meteoroid experienced a simple one-stage exposure history in transit to Earth, calculated to be 1.8 (±0.3) m.y., while the the Taurid complex comets are most consistent with a much more recent disruption event. Further investigations are necessary to better resolve this issue.

From comparisons made between the reflectance spectrum of asteroid (2) Pallas and that of the carbonaceous chondrite groups, it was shown that a close similarity exists to Renazzo. However, it was shown by Marsset et al. (2020) that Pallas along with its large associated family is potentially linked to the CM group—perhaps most notably in having a bulk density (2.89 g/cm^–³) that is the same within error as the grain density of CM chondrites (2.90 g/cm^–³). They suggest that the differences observed in the respective spectra might be explained by the occurrence of heating and dehydration processes on Pallas.

On the other hand, a CRE age study of CM chondrites conducted by Meier et al. (2016) shows a possible relationship exists to the asteroid breakup event ~8.3 m.y. ago that formed the Ch/C/Cg-type members of the Veritas family. In addition to the large abundance of 3He-enriched interplanetary dust discovered in 8.2 m.y.-old deep-sea drill cores, ~1/6 of all CM meteorites have 21Ne-based CRE ages that are consistent with derivation from this catastrophic breakup, while others with significantly younger CRE ages could represent secondary collisions among the Veritas fragments.

In a study comparing the near-infrared spectra of Jovian Trojan asteroids to the RELAB meteorite spectra database, Yang and Jewitt (2011) determined that (3548) Eurybates (Eurybates collisional family) is one of the few Jovian Trojans that have a neutral (gray) spectral slope and are classified as C-type asteroids, rather than the more typical red-sloped D-type Trojan asteroids. At least three Eurybates family Trojans are best matched with both the spectrum and the albedo of CM2 chondrites (exemplar Mighei in diagram below).

Nishiizumi and Caffee (2012) determined the CRE age for over 120 CM2 chondrites based on 10Be and 16Al. They found that most CM chondrites have short CRE ages of <2 m.y., with many of those with CRE ages <1 m.y. comprising two clusters of 0.2 and 0.5-0.7 m.y. In addition, they determined the CRE ages for a number of CM1 and CM1/2 meteorites and one C1/2-ungrouped meteorite, as well as several CI1 meteorites. With few exceptions, the CRE ages for the CM1, CM1/2, and C1/2-ungrouped samples, as well as the CI1 samples in their study, fall into the 0.2 m.y. cluster. These results led to them to infer that the CI and CM parent bodies experienced a mutual collision 0.2 m.y. ago.

Another CM chondrite sampling was utilized for a CRE age and petrographic study subsequently published by Takenouchi et al. (2014) and Zolensky et al. (2017). They contend that these samples comprise four separate CRE age groupings at ~0.1, ~0.2, ~0.6, and ~2 m.y., which could represent separate collisional events (see diagram below). In addition, these investigators recognized that the CM chondrites with the shortest CRE ages experienced the highest degrees of aqueous alteration, and that those with the longest CRE ages are composed of a single lithology (monomict). Plausible explanations for these findings were presented with consideration for both one- and two-parent body scenarios. Murchison has a CRE age of 800,000 years (Macdougall and Phinney, 1977; Caffee et al., 1983) and thus falls into Group 3 of Takenouchi et al. (2014).

In a related study, King et al. (2020) examined both the phyllosilicate fraction (total phyllosilicate abundance / total anhydrous silicate + total phyllosilicate abundance) and the water abundance for nearly three dozen CM chondrites. Based on these results as well as results from their previous O-isotopic study (2018), they consider it very likely that the CM1 + CM1/2 chondrites and the CM2 chondrites represent separate parent bodies. Further CRE age data was obtained by Krietsch et al. (2021) in a noble gas analysis of 39 CM chondrites along with previously reported noble gas data for 26 other CM chondrites. They found the predominant CRE age cluster is at ~0.2 m.y., with other minor peaks at ~1, ~4.5–6, and ~8 m.y.; the ~8 m.y. CRE age cluster is possibly associated with the breakup and formation of the C-type (Ch/C/Cg) Veritas asteroid family 8.3 (±0.5) m.y. ago. In addition, their data does not support the likelihood of a correlation between the CRE age and the petrologic type among the CM chondrites.

A light-colored clast with some affinities to R chondrites was identified in a Murchison sample (Isa et al., 2013, 2014). Further analyses of this clast were conducted by Bischoff et al. (2018 #6217) and Kerraouch et al. (2023 #6250). The clast has a recrystallized texture with 120° triple junctions, and it was determined that both the geochemical and isotopic compositions (O, Cr, Ti) were similar to CM chondrites rather than to R chondrite or brachinite groups (see photo and diagram below). It was determined by Kerraouch et al. (2019, 2023) that the clast has a mineralogy (e.g., glassy nepheline, maskelynite, highly-oxidized organics) consistent with formation under high temperature and pressure conditions. They inferred that the clast was formed at depth within the CM parent body through a fluid metasomatism process induced by impact shock; the clast is considered to be a CM6 lithology.

Another xenolithic clast, the first igneous inclusion ever found in a CM chondrite, was analyzed by Ebert et al. (2019). The pyroxene fragment is located in lithology A of the NWA 12651 breccia and measures about 65 × 78 µm. The mineralogy, REE concentrations, and O-isotopic composition of the fragment reveal that it originated in the CC region of the protoplanetary disk. In general, the fragment is most similar to the CB chondrites and the Milton pallasite, but some important differences in certain aspects prevent any definitive connection (see photo and diagram below).

The specimen of Murchison shown at the top of the page is a 3.1 g cut fragment. A portion of the fragment is covered with a fresh black fusion crust.