Iron meteorites, also called siderites or ferrous meteorites, are a type of meteorite that consist overwhelmingly of an iron–nickel alloy known as meteoric iron that usually consists of two mineral phases: kamacite and taenite. Most iron meteorites originate from planetary cores of ,
The iron found in iron meteorites was one of the earliest sources of usable iron available to , due to the malleability and ductility of the meteoric iron,
Occurrence
Although they are fairly rare compared to the
, comprising only about 5.7% of witnessed falls, iron meteorites have historically been heavily over-represented in
meteorite collections.
This is due to several factors:
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They are easily recognized as unusual, as opposed to stony meteorites. Modern-day searches for meteorites in deserts and Antarctica yield a much more representative sample of meteorites overall.
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They are much more resistant to weathering.
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They are much more likely to survive atmospheric entry, and are more resistant to the resulting ablation. Hence, they are more likely to be found as large pieces.
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They can be found even when buried by use of surface metal-detecting equipment, due to their metallic composition.
Because they are also denser than stony meteorites, iron meteorites also account for almost 90% of the mass of all known meteorites, about 500 tons.
All the largest known meteorites are of this type, including the largest—the
Hoba meteorite.
Origin
Iron meteorites have been linked to
because both have similar spectral characteristics in the visible and near-infrared. Iron meteorites are thought to be the fragments of the cores of larger ancient
that have been shattered by impacts.
The heat released from the radioactive decay of the short-lived nuclides
26Al and
60Fe is considered as a plausible cause for the melting and differentiation of their parent bodies in the early Solar System.
Melting produced from the heat of impacts is another cause of melting and differentiation.
[Wasson, J. T. (1969). The chemical classification of iron meteorites—III. Hexahedrites and other irons with germanium concentrations between 80 and 200 ppm. Geochimica et Cosmochimica Acta, 33(7), 859–876.] The IIE iron meteorites may be a notable exception, in that they probably originate from the crust of
S-type asteroid 6 Hebe.
Chemical and isotope analysis indicates that at least about 50 distinct parent bodies were involved. This implies that there were once at least this many large, differentiated, asteroids in the asteroid belt – many more than today.
Composition
The overwhelming bulk of these meteorites consists of the FeNi-alloys
kamacite and
taenite. Minor minerals, when occurring, often form rounded nodules of
troilite or
graphite, surrounded by
schreibersite and
cohenite.
Schreibersite and
troilite also occur as plate shaped inclusions, which show up on cut surfaces as cm-long and mm-thick lamellae. The
troilite plates are called
Reichenbach lamellae.
[J. G. Burke, Cosmic Debris: Meteorites in History. University of California Press, 1986.]
The chemical composition is dominated by the elements Iron, Nickel and Cobalt, which make up more than 95%. Nickel is always present; the concentration is nearly always higher than 5% and may be as high as about 25%.[J. T. Wasson, Meteorites: Classification and Properties. Springer-Verlag, 1974.] A significant percentage of nickel can be used in the field to distinguish meteoritic irons from human-made iron products, which usually contain lower amounts of Ni, but it is not enough to prove meteoritic origin.
Use
Iron meteorites were historically used for their
meteoric iron, which was forged into cultural objects, tools or weapons. With the advent of smelting and the beginning of the
Iron Age the importance of iron meteorites as a resource decreased, at least in those cultures that developed those techniques. In Ancient Egypt and other civilizations before the
Iron Age, iron was as valuable as gold, since both came from meteorites, for example Tutankhamun's meteoric iron dagger.
The Inuit used the Cape York meteorite for a much longer time. Iron meteorites themselves were sometimes used unaltered as collectibles or even religious symbols (e.g.
Clackamas people worshiping the Willamette meteorite).
Today iron meteorites are prized collectibles for academic institutions and individuals. Some are also tourist attractions as in the case of the
Hoba meteorite.
Classification
Two classifications are in use: the classic structural classification and the newer chemical classification.
[Vagn F. Buchwald, Handbook of Iron Meteorites. University of California Press, 1975.]
Structural classification
The older structural classification is based on the presence or absence of the Widmanstätten pattern, which can be assessed from the appearance of polished cross-sections that have been etched with acid. This is connected with the relative abundance of nickel to iron. The categories are:
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(H): low nickel, no Widmanstätten pattern, may present Neumann lines;
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(O): average to high nickel, Widmanstätten patterns, most common class. They can be further divided up on the basis of the width of the kamacite lamellae from coarsest to finest.
[James H. Shirley, Rhodes Whitmore Fairbridge, Encyclopedia of planetary sciences, Springer, 1997. ]
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Coarsest (Ogg): lamellae width > 3.3 mm
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Coarse (Og): lamellae width 1.3–3.3 mm
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Medium (Om): lamellae width 0.5–1.3 mm
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Fine (Of): lamellae width 0.2–0.5 mm
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Finest (Off): lamellae width < 0.2 mm
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Plessitic (Opl): a transitional structure between octahedrites and ataxites
[Geochimica et Cosmochimica Acta, Volume 45, Ed. 9–12]
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(D): very high nickel, no Widmanstätten pattern, rare.
Chemical classification
A newer chemical classification scheme based on the proportions of the trace elements
Gallium,
Germanium and
Iridium separates the iron meteorites into classes corresponding to distinct
asteroid parent bodies.
[John T. Wasson: Meteorites. Springer-Verlag 1974.] This classification is based on diagrams that plot
nickel content against different trace elements (e.g. Ga, Ge and Ir). The different iron meteorite groups appear as data point clusters.
There were originally four of these groups designated by the Roman numerals I, II, III, IV. When more chemical data became available these were split, e.g. Group IV was split into IVA meteorites and IVB meteorites. Even later some groups got joined again when intermediate meteorites were discovered, e.g. IIIA and IIIB were combined into the IIIAB meteorites.
In 2006 iron meteorites were classified into 13 groups (one for uncategorized irons):
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IAB meteorite
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IA: Medium and coarse octahedrites, 6.4–8.7% Ni, 55–100 ppm Ga, 190–520 ppm Ge, 0.6–5.5 ppm Ir, Ge-Ni correlation negative.
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IB: Ataxites and medium octahedrites, 8.7–25% Ni, 11–55 ppm Ga, 25–190 ppm Ge, 0.3–2 ppm Ir, Ge-Ni correlation negative.
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IC meteorites: 6.1–6.8% Ni. The Ni concentrations are positively correlated with As (4–9 μg/g), Au (0.6–1.0 μg/g) and P (0.17–0.40%) and negatively correlated with Ga (54–42 μg/g), Ir (9–0.07 μg/g) and W (2.4–0.8 μg/g).
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IIAB meteorites
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IIA: Hexahedrites, 5.3–5.7% Ni, 57–62 ppm Ga, 170–185 ppm Ge, 2–60 ppm Ir.
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IIB: Coarsest octahedrites, 5.7–6.4% Ni, 446–59 pm Ga, 107–183 ppm Ge, 0.01–0.5 ppm Ir, Ge-Ni correlation negative.
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IIC meteorite: Plessitic octahedrites, 9.3–11.5% Ni, 37–39 ppm Ga, 88–114 ppm Ge, 4–11 ppm Ir, Ge-Ni correlation positive
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IID meteorite: Fine to medium octahedrites, 9.8–11.3%Ni, 70–83 ppm Ga, 82–98 ppm Ge, 3.5–18 ppm Ir, Ge-Ni correlation positive
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IIE: octahedrites of various coarseness, 7.5–9.7% Ni, 21–28 ppm Ga, 60–75 ppm Ge, 1–8 ppm Ir, Ge-Ni correlation absent
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IIIAB meteorites: Medium octahedrites, 7.1–10.5% Ni, 16–23 ppm Ga, 27–47 ppm Ge, 0.01–19 ppm Ir
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IIICD meteorite: Ataxites to fine octahedrites, 10–23% Ni, 1.5–27 ppm Ga, 1.4–70 ppm Ge, 0.02–0.55 ppm Ir
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IIIE meteorites: Coarse octahedrites, 8.2–9.0% Ni, 17–19 ppm Ga, 3–37 ppm Ge, 0.05–6 ppm Ir, Ge-Ni correlation absent
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IIIF meteorites: Medium to coarse octahedrites, 6.8–7.8% Ni,6.3–7.2 ppm Ga, 0.7–1.1 ppm Ge, 1.3–7.9 ppm Ir, Ge–Ni correlation absent
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IVA meteorites: Fine octahedrites, 7.4–9.4% Ni, 1.6–2.4 ppm Ga, 0.09–0.14 ppm Ge, 0.4–4 ppm Ir, Ge-Ni correlation positive
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IVB meteorite: Ataxites, 16–26% Ni, 0.17–0.27 ppm Ga, 0,03–0,07 ppm Ge, 13–38 ppm Ir, Ge–Ni correlation positive
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Ungrouped meteorites. This is actually quite a large collection (about 15% of the total) of over 100 meteorites that do not fit into any of the larger classes above, and come from about 50 distinct parent bodies.
Additional groups and grouplets are discussed in the scientific literature:
Magmatic and nonmagmatic (primitive) irons
The iron meteorites were previously divided into two classes: magmatic irons and non magmatic or primitive irons. Now this definition is deprecated.
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| Nonmagmatic or primitive iron meteorites | IAB meteorites, IIE |
| Magmatic iron meteorites | IC, IIAB, IIC, IID, IIF, IIG meteorites, IIIAB, IIIE, IIIF, IVA, IVB meteorites |
Stony–iron meteorites
There are also specific categories for mixed-composition meteorites, in which iron and 'stony' materials are combined.
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Stony–iron meteorites
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Main group pallasites
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Eagle station pallasite grouplet
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Pyroxene Pallasite grouplet
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Mesosiderite group
==Gallery==
, the biggest known iron meteorite. It lies in
Namibia and weighs about 60 tons.]]
, class IIAB). This specimen is about wide.]]
meteorites.]]
See also
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Glossary of meteoritics
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Hraschina meteorite
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Meteoritics
Notes
External links
