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posted September 30, 2005
Portales Valley: Not Just Another Ordinary Chondrite--- A melted meteorite gives a snapshot of the heat and shock that wracked an asteroid during the first stages of differentiation.
Written by Alex Ruzicka and Melinda Hutson
Differentiation: a widespread but poorly-understood process
Most solar system material underwent differentiation, a process involving melting and separation of liquids and solids of varying density and chemical composition. However, chondritic meteorites escaped this process and are believed to be pieces of undifferentiated asteroids. All other meteorites, and probably all rocks from planets and large moons, melted when the parent bodies differentiated to form cores, mantles, and crusts. The heat source for differentiation is uncertain, as are the exact physical processes and conditions that allowed differentiation to proceed in small planetary bodies with weak gravity. Proposed sources of heat include internally-generated heat from short-lived radioactive materials such as aluminum-26 (26Al), external heating from our young active Sun, and heating resulting from collisions between planetary bodies (shock heating). A detailed study of the Portales Valley meteorite [Data link from Meteoritical Database] suggests that differentiation of small planetary bodies involved a combination of an internal heat source and shock. Shock heating was not the major heat source involved in differentiation, but the stress waves associated with even modest shock events played a critical role in helping materials to separate and reconfigure during differentiation.
A sequence of images showing stages in the differentiation of a planetesimal, an early-formed planetary body. The image in the left hand side shows a chondritic planetesimal becoming hot enough for melting to begin. The middle image shows that the heavier metallic liquid sinks toward the center, while the less dense rocky material rises toward the surface. The result is a differentiated object with a crust, mantle and core, as shown in the image in the right hand side. (Images created by Frank Granshaw of Artemis Software for the Cascadia Meteorite Laboratory, Portland State University.)
Not an ordinary H6 ordinary chondrite
Three features link Portales Valley to H-group ordinary chondrites. These are (1) the presence of rare chondrules with a rather typical chondritic texture present in silicate-rich areas, (2) the compositions of most minerals, and (3) the bulk oxygen isotopic composition of the meteorite. Nonetheless, Portales Valley contains unusual features that distinguish it from any other ordinary chondrite. Even in a cut section, the differences between Portales Valley and a typical H-chondrite are readily apparent (see figures below).
A comparison of a typical H-chondrite and Portales Valley. Bright areas are mainly metallic; dark areas are mainly silicates. Left: A slice of a meteorite that is paired with the Franconia (H5) chondritic meteorite. The small lines on the ruler are one millimeter apart. Right: A slice of the Portales Valley meteorite showing that the chondritic, silicate-rich material occurs as angular clasts floating in metallic veins. Tiny bright spots in silicate-rich clasts consist of troilite (FeS) and smaller amounts of fine-grained metal. A large graphite nodule is visible.
Besides the obvious differences between Portales Valley and a typical H chondrite, Portales Valley is also unusual in several other ways. It is the only known ordinary chondrite that contains coarse (cm-sized) graphite nodules as well as metal that shows a Widmanstätten texture (an intergrowth of high- and low-Ni metal, see left image below), both of which are common in iron meteorites. Another notable feature is that different sections of Portales Valley vary widely in their proportion of metal, ranging from silicate-rich areas almost devoid of metal to areas that are almost entirely metal. Finally, Portales Valley is also unusual in having coarse (0.5-1 mm across) and abundant phosphate minerals, which are usually found at the contact between metal and silicate-rich areas (see right image below).
These are back-scattered electron images of areas in Portales Valley. Left: Metal vein showing parallel kamacite (low-Ni metal) lamellae surrounded by higher Ni-metal (zoned taenite and plessite), representing a Widmanstätten texture similar to that found in iron meteorites. The entire metal grain is swathed by kamacite. Right: Coarse phosphate (merrillite) intergrown with silicates (plagioclase, orthopyroxene, olivine) next to coarse FeNi-metal (white).
Varied interpretations of Portales Valley
Portales Valley has been alternately interpreted as an annealed (heated) impact breccia, a primitive achondrite, or a meteorite transitional between chondrites and silicate-bearing iron meteorites. It is important to determine which, if any, of these ideas is correct, as each implies a different heat source and formation mechanism for the meteorite. We will consider each of these ideas below.
Annealed impact melt breccia?
One possibility is that Portales Valley represents an impact melt breccia that has undergone slow cooling from high temperatures (annealing). When two objects collide, they may generate enough heat to create a melt, which can form veins that cut through unmelted portions of the meteorite. One model for Portales Valley is that the metal veins were produced by this type of shock melting process. There are some problems with this model. Studies show that shock deforms minerals in a characteristic fashion producing features such as planar fractures and mosaic extinction in olivine and structural changes in feldspars (see PSRD article: Asteroid Heating: A Shocking View.) None of these deformation features are observed in Portales Valley. It has been proposed that deformation features were present originally but were removed by annealing. Even so, there are other problems with this model. Typically when a chondrite is partially melted, glassy silicate veins are produced which cut through unmelted material (see right image below). With more extensive shock melting, larger areas of melt are produced, with metal and troilite forming globules embedded in silicate melts (see left image below). In neither case are large metallic veins produced. Another problem is that in order to produce the large metal veins observed in Portales Valley, temperatures would have to have been so high that the silicates would be substantially melted and there would be no visible chondritic texture left.
These meteorites show features not seen in Portales Valley. The bright areas are mainly metallic; the dark areas are mainly silicates. Left: "Gao melt" showing clasts of H6 material surrounded by metal-bearing silicate shock melt. The metal in the melted portion forms droplets instead of veins (field of view is ~4.5 cm wide). Right: Peekskill (H6) chondrite, which consists of angular clasts surrounded by thin, dark glassy melt veins.
Another possibility is that Portales Valley is a primitive achondrite, such as an acapulcoite, lodranite, or winonaite. These are meteorites that are approximately chondritic in chemical composition, but which have been raised to high enough temperatures to be melted. The primitive achondrites are believed to have been heated solely or primarily by internal heating. They generally do not have any significant vein structure, although one acapulcoite (Monument Draw) contains a coarse phosphate vein and a thin metal vein. Neither of these closely resemble the large vein structure in Portales Valley. Additionally, experiments show that melting chondrites by internal heat alone generally produces isolated patches or globules of metallic melt, not veins.
Bright regions in these meteorites are mainly metallic; dark areas are mainly silicates. Note that the textures of the two meteorites are completely different. Left: NWA 1058, an ungrouped primitive achondrite. Right: Portales Valley. The medium gray object inside the bright metal is one of two graphite nodules found in the meteorite.
Silicate-bearing iron meteorite?
Yet another possibility is that Portales Valley represents a silicate-bearing iron meteorite. Some iron meteorites, such as Campo del Cielo (IAB iron), contain regions that are texturally similar to Portales Valley, as shown in the pictures below. The silicate regions in IAB iron meteorites are often approximately chondritic in composition and mineralogy, but it is clear that Portales Valley is not simply another IAB iron as its oxygen isotope composition is completely different.
This comparison between a silicate-bearing iron meteorite and Portales Valley shows that they are texturally similar. Bright areas are mainly metallic; dark areas are mainly silicates. Left: Campo del Cielo - IAB silicate-bearing iron. Right: Portales Valley.
On the other hand, the oxygen isotope composition of Portales Valley is the same as that of H-group ordinary chondrites and resembles the IIE group of silicate-bearing iron meteorites, as shown in the diagram below. The silicate-bearing IIE iron meteorites are a diverse group. Some contain silicates that are not similar to chondrites in composition at all. Three others (Netschaëvo, Techado, and Watson) contain silicates that are approximately chondritic in mineralogy and bulk chemical composition. Two of these (Netschaëvo and Techado) also contain a few recognizable chondrules, similar to Portales Valley. Despite these similarities, there are significant differences in mineral compositions and abundances between Portales Valley and IIE irons such as Netschaëvo. These differences suggest that Portales Valley is not simply another silicate-bearing IIE iron meteorite.
Standard three-isotope oxygen diagram showing the compositions of Portales Valley, H-, L-, and LL-group ordinary chondrite, and IIE iron meteorites. TF is the terrestrial fractionation line. The y-axis plots the ratio of oxygen-17 to oxygen-16 compared to mean sea water. The x-axis is the ratio of oxygen-18 to oxygen-16, also normalized to sea water. This figure shows that there is an overall resemblance between Portales Valley, H-group chondrites, and IIE iron meteorites.
So how did Portales Valley form?
The best model for producing Portales Valley involves a blend of the three possibilities described above. A shock process was probably responsible for producing the obvious coarse vein structure, as experiments show that such veins cannot be produced easily by static heating. However, such a shock event could not have been very intense, as the minerals in the meteorite are not significantly deformed. On the other hand, as with primitive achondrites and iron meteorites, there is clear evidence that portions of Portales Valley melted, probably by an internal heating mechanism unrelated to shock. The reason that Portales Valley is difficult to pigeonhole is that it is transitional between primitive H-chondrite-like material and more evolved (achondrite, iron) meteorite types. Because it is transitional, Portales Valley provides a snapshot of the first stages of differentiation in asteroids.
Many unusual features of Portales Valley provide clues as to how it formed, and any story of its formation has to explain them. These features include:
Melted and mobilized metal and sulfide
There is good evidence that at least some of the metal and troilite in Portales Valley was molten. The prominent metal-veining textures imply that metal was substantially molten and that it sometimes entrained silicate fragments (clasts) that floated in the metal. Moreover, the composition of the metal is somewhat different than that found in H-chondrites, and this difference can be explained by a partial melting process.
The trace-element composition of the metal in Portales Valley varies between the metal present in the coarse veins, and that found as finer grains in silicate-rich areas. A model involving partial melting of metal and sulfide with incomplete separation of melted and solid portions can explain this variation and also provides constraints on the maximum temperature during melting. The graphs below compare the composition of metal in coarse veins and silicate areas (filled squares and open circles, respectively) to model compositions (lines) produced by melting either 33% or 50% of the metal and sulfide in an H-chondrite, while keeping the melt in chemical equilibrium with the solid. Shock processes cause the melt to move through the meteorite, relative to the solid. Solid and liquid metal can be mixed in different proportions in various places in the meteorite. In the figure below, the different lines indicate various proportions of solid metal fractions (given by Xsolid, where Xsolid can be as low as zero or as high as one) relative to the total amount of metal (liquid or solid). The compositions are normalized to the abundance of nickel and to H-chondrites. With 33% melting, a solid-liquid metal mixture containing ~20-40% solid agrees with the observed composition of fine metal in Portales Valley, and a mixture containing ~40-80% solid substantially agrees with the composition of the coarse vein metal. The Ga/Ni ratio of the latter is too high to be explained by the model, but the concentration of Ga is known to be affected by shock, which could account for this discrepancy. In contrast, with 50% melting, the models clearly fail to match the observed compositions. The model results imply that metallic melt fractions of less than or equal to 40% provide acceptable matches to the chemistry of Portales Valley. This amount of melting corresponds to temperatures of ~940-1150 oC. With these temperatures, as much as 13% of the silicates could have melted as well.
These complicated, but informative, diagrams combine data from the Portales Valley meteorite (symbols) with theoretical calculations. The graph on the left shows how the ratios of the concentrations of several elements in the metallic iron vary with the amount of solid and liquid metal present. The data match reasonably well for 20-80% solid metal if the amount of melting was 33% (as shown in the left graph). The data do not match at all if 50% of the metal was molten (as shown in the right graph).
The inferred temperatures of ~940-1150 oC for Portales Valley are somewhat higher than the maximum temperatures of ~800-960 oC reached by H-chondrites (type 6 metamorphic grade) due to internal heating. The most likely explanation for the features seen in Portales Valley is that it experienced a shock event while it was already warm from internal heating. The shock would have provided only a small temperature increase. More importantly, the shock wave was necessary for moving melt through the meteorite. Portales Valley probably formed at depth in the parent body below an impact crater in a slowly-cooling environment, enabling the Widmanstätten structure to form in metal and allowing other mineralogical reactions to proceed.
When a chondrite is partially melted, all of the sulfide phases will melt and the sulfur will be concentrated in the metallic melt. The modeling results shown in the graphs above indicate that the metallic regions in the silicate-rich areas had a higher proportion of liquid metal, and thus should have incorporated more sulfur than the coarse metal veins. In agreement with this, troilite, the major sulfur-bearing phase in Portales Valley, is indeed concentrated in silicate-rich areas and not found in coarse metal vein areas. However, the models imply that at least some sulfur should have been present in the coarse veins initially, when metallic liquid was still present. The absence of troilite in the coarse veins implies that sulfur-bearing metallic liquid must have been expelled from the coarse veins, and moved into the silicate-rich areas, before Portales Valley finished solidifying.
Changes in mineralogy due to mobilization of metal and sulfide
The presence of metallic liquids and the transport of this liquid through the Portales Valley source region had a dramatic effect on the distribution and amount of minerals in the remaining rock. For example, carbon, like sulfur, will dissolve in metallic liquids during partial melting. In order to account for the centimeter-sized graphite nodules found in the meteorite, carbon must have been scavenged from large volumes and concentrated locally in the metallic liquid, where it crystallized to form the nodules. A similar crystallization process was probably responsible for making graphite nodules in iron meteorites. The scavenging effect inferred for Portales Valley would have been facilitated by the presence of moving metallic liquids, which passed through large volumes of the rock, picking up carbon along the way.
Moreover, at the high temperatures inferred for Portales Valley, phosphorus would have dissolved in metallic alloy. Upon cooling, phosphorus-bearing metal will react with high-calcium pyroxene in the silicates to produce phosphates such as merrillite and apatite. This reaction can explain why phosphate minerals are preferentially concentrated at metal-silicate interfaces in Portales Valley, and why phosphate is enriched and clinopyroxene is depleted in Portales Valley compared to ordinary chondrites. Thermodynamic analysis suggests that the phosphate would have been produced between temperatures of 975-725 oC as the meteorite cooled slowly from high temperatures. Finally, the phosphate-forming reactions redistributed oxygen, which changed the proportions of the major silicate minerals (olivine and pyroxene) in the meteorite. The figure below shows the olivine-to-pyroxene ratio and metal content in Portales Valley compared to other meteorites. Typically the olivine/pyroxene ratio in Portales Valley is lower than that found in H-chondrites. As shown by the dashed line, there is a relationship between metal content and olivine/pyroxene ratio in Portales Valley, forming a trend which is unlike that found in H-chondrites and acapulcoites (a primitive achondrite). Areas in Portales Valley that contain more metal are areas in which there was a greater amount of phosphorus available for reaction, resulting in lower olivine contents.
This diagram shows that the ratio of olivine to low-calcium pyroxeme is lower in Portales Valley than that found in H-chondrites.
|Feature in Portales Valley||Proposed Formation|
|silicates trapped in metallic veins||metal melted and flowed because of shock heating|
|metal composition different from H-chondrites||metal compositions were modified by partial melting|
|FeS concentrated in silicate areas||sulfur-bearing metal was expelled from coarse metal veins|
|large graphite nodules in metallic veins||carbon was scavenged from wide area and concentrated in metal|
|big phosphate grains next to metal||phosphorus in the metal moved to the contact between the metal and silicate and was oxidized|
|low content of high-calcium pyroxene||formation of calcium phosphate occurred by reaction with high-calcium pyroxene|
|low ratio of olivine to low-calcium pyroxene||formation of phosphate minerals redistributed oxygen in the silicates, leading to the destruction of olivine and the formation of low-calcium pyroxene|
The complexities of planet formation
Portales Valley is transitional between primitive (chondrite) and evolved (achondrite and iron) meteorites. It formed by a shock event while the parent body was being heated internally. Portales Valley can be considered an achondrite in the sense that it was partially melted. It also bears striking resemblances to silicate-bearing iron meteorites, which formed by differentiation. The main importance of Portales Valley may ultimately lie in what the meteorite has to tell us about the formation of other kinds of meteorites and the parent bodies from which they were derived. Portales Valley may be telling us that simultaneous impact and internal heating events could have been important in the overall process of differentiation. The meteorite gives us a glimpse at the nature of the complex processes that operated in even small bodies as the planets were forming.
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