Collisional Disruption of a Primary Planetary Body
On one scale of Solar System history, the nascence of planetesimal formation spanned less than 100 m.y. The most active period was determined to be the first 1020 m.y., just after Jupiter and Saturn had formed and the protoplanetary disk was void of its gas shroud (Davison et al., 2013). During this time a dynamical, stochastic, collisional evolution played outcollisional growth proceeded in the face of ongoing disruptive impact events on contemporaneous accreting bodies. A number of these growing planetesimals accumulated heat through energetic impacts and the decay of radiogenic elements such as 26Al, beginning a stage of gravitational differentiation into a crust, silicate mantle, and metallic core. Some of the larger planestesimals developed a rotating core dynamo producing a weak magnetic field, as evidenced by the paleomagnetic signature detectable today in their associated meteorites.
Davison et al. (2013) calculated that during the first 100 m.y. only a very few planetesimals (<~50) were able to grow to very large sizes, in the range of 200600 km in diameter, without experiencing a disruptive collision. At the same time, there is meteoritical evidence that suggests a few planetesimals grew to protoplanetary (or even planetary) sizes before experiencing a disruptive collision; i.e., an impact by an object typically >~60 km in diameter traveling ~1825 km/s. As an example, it was proposed by Irving et al. (2009) that the diverse meteorite lithologies with similar O-isotopic compositions to the HED clan of meteorites, generally considered to be derived from the asteroid 4 Vesta, were once part of an even larger former differentiated planetary body which they named "Opis" (the mother of Vesta in Greek mythology).
Another such hypothesized collisionally-disaggregated planetary body (here named "Antaeus") was conceived by Irving et al. (2004) to have comprised many diverse lithologies, here expanded upon to include the following: a metallic core region composed of IIF-type iron like Del Rio (Kracher et al., 1980), IVB-type iron like Santa Clara and/or South Byron trio-type iron (Corrigan et al., 2017; Hilton et al., 2018); a coremantle boundary or upper mantle impact-melted zone composed of a metal+silicate assemblage that corresponds to the Eagle Station group and/or the Milton pallasite (Corrigan et al., 2017; Sanborn et al., 2018), along with the NWA 176 (related to Bocaiuva; Liu, 2001) silicated iron; a dunitic mantle zone possibly represented by NWA 7822; an intensely thermally-metamorphosed stratigraphy resembling the NWA 3133 and NWA 10503 metachondrites (Irving et al., 2004; Irving et al., 2016; Sanborn et al., 2018); and a thick insulating crust (~20 km; Davison et al., 2013), possibly involving a late accetionary stage, comprising a primitive chondruleCAI-rich regolith consisting of several distinct lithological zones comprising reduced Allende-like, oxidized Allende-like, and highly aqueously-altered Bali-like material. The detailed petrogenetic sequences by which each of these meteorites acquired their present form, and the question as to whether these events occurred before, during, or after a catastrophic disruption of the primary planetary body (or were associated with post-disruption daughter objects), are subjects that are still under investigation.
Importantly, the O- and Cr-isotopic signatures of Eagle Station have been utilized to establish an early formation age of 4.557 b.y., or 11 m.y. years after CAI formation. According to Dauphas et al. (2005), application of the HfW isotopic chronometer to Eagle Station also gives a relatively late metalsilicate segregation for Eagle Station of ~10 m.y. after differentiation of the HED parent body 4 Vesta (which occurred as early as 1.3 m.y. after CAI formation; Schiller et al., 2010). Since it has been calculated that melting and coremantle differentiation due to radiogenic heating should cease after ~78 m.y. (Sahijpal et al., 2007), it may be inferred that heating of the Eagle Station asteroid continued until after all radiogenic 26Al and 60Fe was extinct, and that such late heating would have been generated through large impact events. In support of that reasoning, John T. Wasson (2016) presented evidence that the slow heating generated entirely by the decay of 26Al is insufficient to melt asteroids, and that an additional heat source would have been required; e.g., the rapid heating incurred from major impact events. He determined that the canonical 26Al/27Al ratio of 0.000052 is much too low to cause any significant melting, and that a minimum ratio of 0.00001 would be required to produce a 20% melt fraction on a well-insulated body having a significant concentration of 26Al. For example, the initial ratio of 0.00000040.0000005 calculated for the angrites Sah 99555 and D'Orbigny based on their 26Al26Mg isochrons is too low to have generated any significant melting without an additional heat source. Therefore, impacts were a major source of heating in early solar system history.
Likewise, the formation scenario envisioned for the silicated irons NWA 176 and Bocaiuva is consistent with impact-heating events on a small-sized asteroid. The final mixing event was accompanied by an initial rapid-cooling stage beginning at the metalsilicate equilibrium temperature of ~1100°C, and was sustained down to ~600°C. This was followed by a slow cooling stage in which a Thomson (Widmanstätten) structure was formed (Desnoyers et al., 1985). Another fast cooling stage was initiated between approximately 600°C and 300°C as indicated by the absence of tetrataenite and other petrographic features (Araujo et al., 1983). There are major structural similarities between the NWA 176 and Bocaiuva silicated irons and those silicated iron members of the IIE and IAB complex iron groups. This suggests that similar impact processes, such as a catastrophic breakup event, occurred on each of these relatively small, nonmagmatic parent bodies; however, only the IIF irons and the Eagle Station pallasites share any significant geochemical similarities with NWA 176 and Bocaiuva (Bunch et al., 1970; Curvello et al., 1983). Notably, NWA 176, Bocaiuva, and the Eagle Station pallasites, as well as other distinct meteorite lithologies, have similar O- and/or Cr-isotopic compositions to the CV chondrites (Clayton and Mayeda., 1996; Liu et al, 2001; Shukolyukov and Lugmair, 2001). Taking the many similarities into account, it seems possible that these otherwise disparate meteorites originated on a common chondritic precursor parent body (Malvin et al., 1985).
In an effort to better resolve potential genetic relationships that might exist among the meteorites mentioned above associated with the hypothetical Antaeus, a Cr-isotopic analysis of olivine from the Milton pallasite was conducted by Sanborn et al. (2018). It is demonstrated on a coupled Δ17O vs. ε54Cr diagram (shown below) that Milton plots among the CV clan and plausibly shares a genetic relationship, but also that Eagle Station plots closer to the CK (or CO) chondrite group. It could be inferred that both the CV and CK planetesimals experienced a similar petrogenetic history in a similar isotopic reservoir of the nascent solar system.
Chromium vs. Oxygen Isotope Plot
click on diagram for a magnified view
Diagram credit: Sanborn et al., 49th LPSC, #1780 (2018)
Notably, a formation scenario for pallasites was proposed by Asphaug et al. (2006) and Danielson et al. (2009) in which the wide variation in metalsilicate textures and bulk compositions that is observed among MG pallasite members is the result of a grazing collision between partially molten planetary embryos. They assert that such a collision resulted in the formation of a chain of smaller objects having diverse compositions. It may be more than coincidental that the O-isotopic composition of the Milton pallasite plots proximate to the trend line of the Eagle Station group pallasites (now termed the Allende Mixing line: slope = 0.94 ±0.01). Both of these rapidly-cooled pallasites contain high concentrations of the refractory siderophile element Ir relative to main-group (MG) pallasites (Jones et al., 2003), and they both have overlapping Fe and Ni abundances (wt%) in their metal component; however, significant variations observed in their minor and trace element concentrations indicate that they each experienced different crystallization processes (Hillebrand, 2004). Still, there is a good possibility that one or both of these pallasites did share a common precursor parent body with the CV clan of meteorites, at least prior to any collisional disruption event.
Diagram adapted from Korochantsev et al., 44th LPSC, #2020 (2013)
With the advent of better investigative techniques, scientists have explored the possibility of a genetic relationship between IVB irons and other meteorite groups based on O-isotopic analyses. Utilizing chromite grains from IVB irons Warburton Range and Hoba, Corrigan et al. (2017) found that IVB irons share close similarities to the South Byron trio irons (Babb's Mill [Troost's], South Byron, and Inland Forts [ILD] 83500)Milton pallasite grouping (MSB in diagram below). Moreover, the O-isotopic compositions of the IVB irons and the South Byron trioMilton grouping fall within the range of the oxidized CV and CK chondrites.
Diagram credit: Corrigan et al., 48h LPSC, #2556 (2017)
Subsequent to the catastrophic disruption of the primary planetary body that is envisioned here, and the sorting and re-accretion of material into a number of daughter objects, multiple impacts onto these small asteroids could have led to the formation of sub-surface melt pools tens of meters in size. Differentiation of these melt pools would have resulted in cumulus olivine sequestered above a metal layer, and an olivine residuum that had drained below this metal layera complex assemblage from which associated pallasitic and silicated-iron lithologies could be derived thereafter during less-energetic, rapidly-cooled impact events (Malvin et al., 1985). The anomalously-high Ir contents measured in some of the associated metalsilicate mixtures (e.g., Eagle Station group, Milton) and segregated metal regions (IIF irons, South Byron trio) would be consistent with metal that crystallized at the lowest levels of the melt chamber. Such late-stage, rapidly-cooled, impact-heating events could have allowed for the retention of the original O- and Cr-isotopic composition of the primary planetary body (Humayun and Weiss, 2011 and references therein). The differences that exist in δ54Cr between chromite and olivine in the Eagle Station pallasite, but which are not observed in CV chondrites, could be the result of a distinct Cr source associated with impact projectile(s) which eventually led to the formation of the Eagle Station-type pallasites and other related lithologies (Papanastassiou and Chen, 2011).
On an oxygen three-isotope diagram (see example below), the CO chondrites plot along the Allende Mixing trend line (former CCAM line), overlapping near the middle of the CV chondrite field. There is a possibility that the CO chondrite group, of which Isna is a highly metamorphosed example (type 3.75), is also implicated in the sequence of events that led to the formation of the diverse CV clan of meteorites as outlined aboveperhaps as another of the daughter objects that accreted after a catastrophic disruption of the primary planetary body. It is also significant that the most unequilibrated CO3 chondrites have isotopic compositions that are similar to anhydrous silicates in meteorites of the CM group, a group with which it also shares many chemical and petrographic similarities. In fact, the CO and CM groups may represent different degrees of low-temperature aqueous alteration of common precursor material which was initially similar to the primitive CO chondrites DOM 08006 (3.003.01) and ALHA77307 (3.03) (Clayton and Mayeda, 1999). Although it is still unresolved whether or not these two groups share a common parental source object, they both represent material from the same nebular region located beyond 3 AU (Wasson, 1988; Rubin, 2010).
Diagram credit: Irving et al., 79th MetSoc, #6461 (2016)
Beyond that, new O-isotopic analyses conducted by Greenwood et al. (2014) on a large sampling of CM chondrites led them to suggest that a possible group relationship (same parent body) may exist between the CM and CO chondrites, previously considered to constitute a clan (groups formed at a similar heliocentric distance) based on early research on refractory lithophile abundances, chondrule size and composition, and O-isotopic composition of high-temperature phases (Kallemeyn and Wasson, 1979, 1981). Moreover, it was found that the matrix component in meteorites of both groups have nearly identical minor element compositions (Greenwood et al., 2014, reference therein). Despite the hiatus that occurs between the CM and CO groups on an oxygen three-isotope diagram, their additional data clearly shows that the CM O-isotopic trend line intersects the CO field, and they have posited a new theory based on the premise that both groups formed on a common parent body. They suggest that the CO group could represent an inner anhydrous zone of a parent body larger than ~120 km in diameter, in which the initial accreted hydrous component was rapidly liberated through endogenous heating (radiogenic) and vented to the surface and into space (Fu and Elkins-Tanton, 2013). Conversely, the outer zone represented by the CM group experienced a high degree of aqueous alteration over an extended duration. A compatable scenario was presented by Fu and Elkins-Tanton (2013) in which early accretion (within ~2 m.y. of CAI formation) of a planetesimal of significant size (>120 km in diameter), composed of low-density material akin to the CM chondrites, could experience internal differentiation without eruption of magma to the surface, thereby retaining a primitive hydrated crustal region.
In their comprehensive oxygen isotope study of carbonaceous chondrite groups, Clayton and Mayeda (1999) showed that many ungrouped members plot along the same mixing line and fill the hiatus between the CO and CM fields (see diagram below). They suggest that both CO and CM groups consist of a common anhydrous silicate precursor, while the CM group represents the interaction of this anhydrous precursor with an aqueous reservoir. The ungrouped members are transitional, with variable water:rock ratios as indicated by the tick marks along the mixing line.
Diagram courtesy of Clayton and Mayeda, GCA, vol. 63, p. 2094 (1999)
'Oxygen isotope studies of carbonaceous chondrites'
See also this oxygen three-isotope diagram presented by Jacquet et al., MAPS, vol. 51, #5, p. 862 (2016)
'Northwest Africa 5958: A weakly altered CM-related ungrouped chondrite, not a CI3' (http://dx.doi.org/10.1111/maps.12628)
Further evidence for a possible common COCM parent body was presented by Schrader and Davidson (2016; #1288). They analyzed the Cr content in olivine grain cores of type-II (FeO-rich) chondrules for a number of CM chondrites spanning the full range of petrologic types (e.g., Sutter's Mill [2.0/2.1]... QUE 97990 [2.6]). Utilizing a coupled diagram comparing the mean Cr2O3 content to the standard deviation (σ) of Cr2O3 content, they demonstrated that both the CO and CM thermal metamorphism curves overlap. Their study also shows that thermal metamorphism and aqueous alteration are not coupled. Another coupled diagram presented by Schrader and Davidson (2016) comparing the Fe and Mn contents of the type-II chondrules among the CM samples is also consistent with a common COCM parent body. Nevertheless, further studies by Schrader and Davidson (2017) led to the development of multiple lines of evidence which indicate that these two groups derive from separate parent bodies.
Moreover, a comparitive analysis of CM and CO chondrites led Chaumard et al. (2018) to the conclusion that both of these groups formed in a common isotopic reservoir and accreted identical anhydrous precursor material comprised of the same two type I chondrule populations: 1) Δ17O ~ 2.5, Mg# <96, and 2) Δ17O ~ 5, Mg# >98.5. Both CM and CO chondrites also accreted identical type II chondrule populations. However, they recognized the many other characteristics that indicate a formation for these two groups on separate parent bodies, including differences in chondrule size (0.15 and 0.30 mm for CO and CM, respectively), matrix abundance (3035 and 70 vol% for CO and CM, respectively), abundance of type II chondrules that contain relict olivine grains (~48% and 1225% for CO and CM, respectively), average CRE age (22 [±18] and 2.8 [±3.1] m.y. for CO and CM, respectively), accretion age (~2.12.7 and ~3.55.0 m.y. after CAIs for CO and CM, respectively), and in abundance of hydrous phases (ice:rock ratio of ~0.10.2 and ~0.30.6 for CO and CM, respectively). They propose a scenario in which the snow line moved inward during the time interval between the accretion at nearly the same location (~23 AU) of these two distinct planetesimals.
Diagram credit: Chaumard et al., GCA, vol. 228, p. 220242 (1 May 2018)
'Oxygen isotope systematics of chondrules in the Murchison CM2 chondrite and implications for the CO-CM relationship'
A scenario compatable with the single parent body hypothesis was presented by Fu and Elkins-Tanton (2013). They propose that early accretion (within ~2 m.y. of CAI formation) of a planetesimal of significant size (>120 km in diameter) and composed of low-density material akin to the CM chondrites could experience internal differentiation without eruption of magma to the surface, thereby retaining a primitive hydrated crustal region. It could be deduced that a catastrophic disruption resulted in re-accretion of material into numerous daughter objects, which subsequently experienced impact-ejection of material into storage orbits within the outer asteroid belt. Further fragmentation events (collisional cascade processes), along with the Yarkovsky effect, would have delivered samples into mean motion resonances with some fragments eventually achieving Earth-crossing orbits.
The hypothesis of multiple daughter objects being formed following the catastrophic disruption of a large, partially differentiated primary planetary body could allow for the potential inclusion of several less closely-related meteorites. These may include the high-Ni irons of the South Byron trio (South Byron, ILD 83500, and Babb's Mill), which have metallographic compositions (especially siderophile element patterns) and structures similar to the metal in Milton, including kamacite spindles and associated schreibersite, consistent with their formation on the same parent body (Reynolds et al., 2006). These three irons and the metal component in Milton experienced a similar oxidation history during formation; they each have similar depletions of easily oxidized elements as well as similar abundances of siderophiles (McCoy et al., 2008). In addition to the irons mentioned above, several other ungrouped ataxites may be genetically related to this high-Ni iron group, including El Qoseir, Illinois Gulch, Morradal, Nordheim, and Tucson (Kissin, 2010). However, significant differences that exist between their refractory element contents compared to those of the South Byron trio requires further work to establish a specific relationship.
The metal in each of these high-Ni iron meteorites and in Milton is consistent with early crystallization from a metallic-melt phase that experienced a low degree of fractionation. Similarly, the FeNi-metal component of one member of the Eagle Station grouplet, Itzawisis, was derived from a metallic-melt source consistent with that of a differentiated, oxidized-CV source before 20% fractionation had occurred. In a like manner, the metal in Eagle Station derives from a 20% fractionated source (Humayun and Weiss, 2011), while another member of the grouplet, Cold Bay, was shown to derive from a melt source that crystallized after 40% fractionation. The most recent member of the Eagle Station grouplet to be analyzed, Karavannoe, crystallized from an even more evolved metallic-melt that had undergone >60% fractionationthough still not as evolved as the source melt from which MG pallasite metal crystallized. Karavannoe FeNi-metal has a lower Ni content than the other members of the grouplet (Korochantsev et al., 2013), and measurements show that its Ir content is intermediate between that of Eagle Station and Milton.
Further evidence for a large differentiated planetary body having CV-trends lies in the fact that CV chondrites acquired a strong unidirectional natural remanent magnetization ~9 m.y. after CAI formation, reflecting the existence of an internal core dynamo (e.g., Weiss et al., 2010; Elkins-Tanton et al., 2011; Carporzen et al., 2010, 2011; Gattacceca et al., 2013, 2016). Employing multiple investigation techniques, Shah et al. (2017) investigated the paleointensity of 19 Vigarano chondrules and found values of 1.1150 µT. The observed magnetic remanence is considered to have been acquired during brecciation events that occurred ~7 m.y. after initial parent body accretion, with impact shock pressures reaching 1020 GPa. Therefore, they reason that the original paleofield would have been ~40 µT, which is too high to be attributable to the solar wind field, but is in the range of that expected for a planetary core dynamo. As research continues, further evidence for the catastrophic disruption of this former primary body could advance this hypothesis.