Iron meteorites always attract substantial scientific attention because of their unusual composition and structure1,2. Contrary to silicate cosmic material, which is available both from stony meteorites and via delivery by space missions3, iron meteorites have no alternative as a source of information on the phase relationships in the metal-rich zones of celestial bodies2. Phosphide minerals, i.e. those containing phosphorus in an oxidation state lower than zero, play a significant role in the mineralogy of iron meteorites as a component of the ternary Fe–Ni–P system4,5,6,7. Iron-nickel phosphides, though accessory minerals, have paramount influence on the crystallization pathways in iron and stony-iron meteorites8,9. Natural Fe–Ni phosphides are extensively studied as probable carriers of low-valent phosphorus, which was required for the initiation of the prebiotic phosphorylation processes on the early Earth10,11,12,13.

One of the main challenges of planetary science is to obtain insights into the evolution of celestial bodies2. The records of shock events experienced by planetesimals in their space history are preserved in the high-pressure minerals that are retained in meteorites and impact structures14. Unfortunately, the inherent instability of many high-pressure polymorphs under ambient conditions frequently restricts their application to the study of natural objects. In the case of silicate and oxide systems (i.e. stony meteorites and impact craters), the problem is resolved due to a diversity of the high-pressure phases, many of which can be recovered to ambient conditions in the metastable state15,16,17,18. The situation changes dramatically when we are considering the Fe–Ni–P system: there are just two phases that are stable beyond 5 GPa, but that can be metastably preserved upon quenching. These are (1) a high-pressure synthetic counterpart of the mineral zuktamrurite, FeP219,20 and (2) allabogdanite, a high-pressure polymorph of (Fe,Ni)2P21,22. The practical absence of natural high-pressure indicators in the Fe–Ni–P system restricts the recording of the impact history of iron meteorites to indirect evidence, such as shock-induced shear deformation, twinning (Neumann bands) and impact melting1,23 or the extremely rare detection of high-pressure silica polymorphs24. Meanwhile, synthetic allabogdanite-type Fe2P was shown to be stable from 8 GPa to at least 40 GPa of pressure at a temperature above 800 °C, and can be quenched to the ambient conditions22,25. Therefore, allabogdanite, as a natural counterpart of high-pressure Fe2P, could serve as a convenient indicator of shock events in the Fe–Ni–P system, having a stability field similar to that of stishovite (high-pressure rutile-type SiO2)22,26. Like stishovite, which is used as a tracer of shock events in the stony meteorites27,28,29,30, allabogdanite could indicate significant impact events experienced by the iron and stony-iron meteorites.

Unfortunately, until now, allabogdanite was only known to be present in a single iron meteorite, the nickel-rich ataxite Onello21. In the course of ongoing research of the two other nickel-rich ataxites, Santa Catharina and Barbianello, we have confirmed the occurrence of allabogdanite in both of these irons. Herein, we present the results of this current investigation and show that allabogdanite may not be as rare as previously believed, but could often be misidentified as barringerite, a low-pressure polymorph of (Fe,Ni)2P31,32.

The Santa Catharina, Barbianello and Onello meteorites

Santa Catharina

This meteorite was found in 1875 in São Francisco do Sul (Santa Catarina, Brazil)1. The total recovered weight of Santa Catharina, at least 7 metric tons, makes it one of the 15 largest meteorites ever found on Earth1,33. The meteorite is currently classified as an ungrouped iron related to the IAB complex, and structurally related to nickel-rich ataxites34. The latter structural group gathers about 50 iron meteorites having a Ni content exceeding 15 wt.% and featuring a lack of a microscopically resolvable Widmanstätten pattern1,33. Santa Catharina was extensively studied due to a chemical similarity between its metal (~35 wt.% of Ni) and the invar-type alloys (ref.35 and the citing references). More than 50% of the metal matrix of Santa Catharina is composed of 50-50 iron-nickel metal, having an ordered superstructure of the AuCu (L10) type36. The discovery of this mineral, L10-FeNi, now known as tetrataenite37, initiated extensive studies resulting in the development of a new class of permanent magnets38.

Accessory minerals in Santa Catharina are comprised of phosphides related to the schreibersite-nickelphosphide series, Fe3P–Ni3P39,40, sarcopside-like iron phosphate, Fe3(PO4)2, and magnetite39,41. Troilite nodules up to a few centimeters across are very common41. Troilite, FeS, is partially substituted by pentlandite, (Ni,Fe)9S8, and unidentified nickel sulfides41. Phosphide mineralization in Santa Catharina was investigated by several scientific groups using electron microprobe39,41,42, ion microprobe43 and spatially resolved X-ray absorption spectroscopy44. Brandstätter and coauthors42 reported the phosphide mineral corresponding to (Fe,Ni)2P and ascribed it to barringerite, the low-pressure polymorph of (Fe,Ni)2P31, based on its chemical composition.


This small (860 g) ungrouped iron meteorite was found in 1961 in Barbianello, Pavia Province, Lombardia, Italy, and described by Fioretti and Zipfel45. The metal of Barbianello contains ~27 wt.% of Ni and was severely oxidized by the processes of terrestrial weathering. Phosphides in Barbianello were described as schreibersite45, but in fact are represented by its nickel-dominant analogue, nickelphosphide, (Ni,Fe)3P40.


This ungrouped meteorite, found in 1997 in Respublika Sakha (Yakutiya), Russia, is one of the smallest irons ever found (164 g)46,47. The nickel content in Onello varies between 22 and 24 wt.%46. Phosphides are generally represented by the minerals of the schreibersite-nickelphosphide series, Fe3P–Ni3P40,46. Allabogdanite was discovered in this meteorite in 2002 (ref.21) and since that time, it was not known to be anywhere else.


Allabogdanite in the Santa Catharina meteorite

The mineral occurs as lamellar crystals up to 120 μm in length and up to 10 μm thick, which are scattered throughout the meteorite matrix. The cross-sections of neighbouring crystals frequently show a non-random, pseudo-collinear orientation (Fig. 1). Allabogdanite is usually associated with the phosphides related to the schreibersite-nickelphosphide series, Fe3P–Ni3P (Fig. 1). The chemical composition of allabogdanite crystals

Figure 1
figure 1

Lamellar allabogdanite crystals and associated phosphides in the metal matrix of the Santa Catharina meteorite. (a) Photo in reflected light. (b) Image of backscattered electrons (BSE). (cf) Elemental maps of the selected region for (c) nickel, (d) iron, (e) cobalt and (f) phosphorus. The numbering of allabogdanite crystals corresponds to the analyses numbers given in Table 1. Allabogdanite crystal #1 was used for structure determination. Legend: Abg, allabogdanite; Srb, schreibersite; Np, nickelphosphide; Km, kamacite, α-(Fe,Ni).

(depicted in Fig. 1) is summarized in Table 1. Like allabogdanite from the Onello meteorite21, the mineral from Santa Catharina has a uniform chemical composition, shows no signs of chemical zoning and does not interfere with the host Fe-Ni matrix (Fig. 1). Allabogdanite is somewhat enriched in cobalt relative to both Fe-Ni metal and phosphides of the schreibersite-nickelphosphide series (Table 1). The chemical composition and crystal morphology of allabogdanite from Santa Catharina is almost identical to that of barringerite previously described from the same meteorite42. It is highly likely that the “barringerite” reported by Brandstätter and co-authors42 is in fact allabogdanite, as well.

Table 1 Representative chemical composition of allabogdanite and associated minerals.

The crystal structure of allabogdanite from Santa Catharina was determined by an X-ray single-crystal study. It has been solved and refined to R1 = 0.0455, using a tiny fragment of the crystal #1 depicted in Fig. 1. A brief comparison of the crystallographic data of allabogdanite from the Santa Catharina and Onello meteorites is given in Table 2; the detailed crystallographic data are given in the supporting Crystallographic Information File (CIF). The mineral from Santa Catharina is enriched in nickel relative to the allabogdanite from Onello. The higher nickel content results in noticeable shrinkage of the unit cell axes and, consequently, a reduction of the unit cell volume. The overall effect of Fe for Ni substitution is a 1.4% increase in the density of the mineral in Santa Catharina, relative to that from the Onello meteorite.

Table 2 Selected crystallographic data for allabogdanite from the Santa Catharina and Onello meteoritesa.

Allabogdanite in the Barbianello meteorite

Оnly one crystal of (Fe,Ni)2P (Fig. 2) was found in this meteorite, perhaps because of the small available area of the polished section. The size of the allabogdanite crystal (about 7 μm) made the possibility of its safe extraction for the purposes of structure determination doubtful. Therefore, we used the electron backscatter diffraction (EBSD) method for the discrimination between the two possible polymorphs of (Fe,Ni)2P: the low-pressure form, barringerite31, and the high-pressure polymorph, allabogdanite21. The EBSD technique, being inferior to the direct structure solution method, is nevertheless widely used as a non-destructive and highly local method for the purposes of phase diagnostics of micrometer-sized mineral grains30,48. The correctness of identification is determined by the value of mean angular deviation (MAD) between the fitted orientation matrices of the model crystal structure and that of the studied mineral phase. MAD values below 1° are considered reliable. In our case, a MAD of 0.24° was obtained for the allabogdanite structure, whereas no acceptable fit was found for the barringerite model. Therefore, EBSD unambiguously signifies that the studied (Fe,Ni)2P crystal is allabogdanite (Fig. 3).

Figure 2
figure 2

The crystal of allabogdanite residing in the center of the envelope-like kamacite crystal. Kamacite, in due course, is hosted by the taenite single crystal. The thin tetrataenite rim and so-called cloudy zone are visible at the interface between taenite and kamacite. The Barbianello meteorite. (a) Photo in reflected light. (b) Image of backscattered electrons (BSE). The bottom row shows elemental maps for nickel, iron, phosphorus and oxygen, respectively. Legend (Fig. 2) (b): Abg, allabogdanite; α, kamacite [body-centered cubic α-(Fe,Ni)]; γ, taenite [face-centered cubic γ-(Fe,Ni)]; L10, tetrataenite (ordered FeNi); Ox, supergene Fe-Ni oxides.

Figure 3
figure 3

(a) Electron backscatter diffraction (EBSD) Euler orientation map of the Barbianello section depicted in Fig. 2. The red-colored host matrix is a slightly deformed taenite single crystal which is cross-cut parallel to its cube face. The blue-colored envelope is a single crystal of kamacite. Allabogdanite crystal (orange-yellow) resides in the center of kamacite crystal. The black regions indicate unindexed areas. (b) EBSD pattern from the allabogdanite crystal. The mean angular deviation (MAD) is 0.24° (based on 12 Kikuchi bands). (ce) Pole figures showing crystallographic orientation of (c) allabogdanite; (d) kamacite and (e) taenite crystals. Note that [111] axis of kamacite is roughly coincident with [100] axis of taenite. Legend (Fig. 2b): Abg, allabogdanite; α, kamacite [body-centered cubic α-(Fe,Ni)]; γ, taenite [face-centered cubic γ-(Fe,Ni)].

Allabogdanite in the Barbianello meteorite is remarkably distinguished from the mineral found in the Santa Catharina and Onello irons. Firstly, it is significantly enriched in nickel (Table 1). Then, contrary to the former meteorites, in which the mineral is hosted by taenite [face-centered cubic γ-(Fe,Ni)], the allabogdanite crystal in the Barbianello meteorite resides in the center of the kamacite [body-centered cubic α-(Fe,Ni)] field (Fig. 2). The latter, in due course, is comprised of a relatively large (50 × 80 μm) single crystal (Fig. 3) rather than an intergrowth of the randomly oriented grains, called “swathing kamacite”8. The kamacite crystal is embedded into a single crystal of taenite. The coincidence of [111] axis of kamacite with [100] taenite axis (Fig. 3b,c) suggests a non-random, oriented intergrowth of these two phases. The interface from kamacite towards taenite is traced up by the 1–2 μm tetrataenite rim, followed by a 10-μm thick region of Ni-rich metal known as a “cloudy zone”37.


Senateur and coauthors25 first reported that the transition of hexagonal Fe2P (C22-type, Fe2P structure) to the orthorhombic type (C23-type, Co2Si structure) occurs at about 8 GPa and 800 °C. The authors, however, did not determine whether the obtained high-pressure phase is stable or metastable under ambient conditions. A further study carried out by Dera and coauthors22 substantially expanded the P-T stability limits of orthorhombic Fe2P, from 8 GPa to 40 GPa and ~1100 °C. The same authors showed that the high-pressure polymorph of Fe2P is metastable, but can be retained under the ambient conditions and even re-heated to 1100 °C without back transformation to the low-pressure modification. The mineral allabogdanite, C23-type (Fe,Ni)2P, was discovered in the Onello meteorite21, where it contains a significant amount of nickel substituting for iron (Table 1). Therefore, allabogdanite, in a strict sense, is not a natural counterpart of Fe2P, but rather an intermediate member of (Fe1-хNix)2P solid solutions. Because the behaviour of Ni2P under high pressure is completely different from that of Fe2P49, it was not obvious that the pressure-temperature stability limits of pure Fe2P could be extrapolated to natural allabogdanite. Although the results reported by Dera and coauthors22 ruled out the stabilizing effect of Ni on the allabogdanite-type modification of (Fe,Ni)2P, new experimental evidence confirming P-T stability limits of the latter phase would be desirable. These experiments have been recently conducted on the Fe–Ni–P system at a pressure of 6 GPa in the temperature range of 900 to 1100 °C; they did not reveal the existence of allabogdanite-type (Fe,Ni)2P50. Therefore, the lower pressure-temperature stability limit for the high-pressure modification of (Fe,Ni)2P lies beyond 6 GPa and 900 °C, in good agreement with the data obtained for pure high-pressure Fe2P.

Based on the currently available experimental background, natural allabogdanite can now be considered a high-pressure and high-temperature phase, which can be metastably retained upon quick quenching to ambient conditions. It is noteworthy that the maximum recorded nickel content in allabogdanite from the Onello (0.50 Ni atoms per formula unit, apfu), Santa Catharina (0.65 Ni apfu) and Barbianello (0.84 Ni apfu) meteorites significantly exceeds the allowed Ni content predicted by the theoretical calculations for the high-pressure form of (Fe,Ni)2P51. Therefore, it is likely that further experiments will shift the upper limit of the pressure-temperature stability area of allabogdanite towards higher P-T parameters.

The remarkable similarity between the high-pressure polymorphism of Fe2P and silica phases was mentioned by Dera and coauthors22. In this respect, allabogdanite can be considered a convenient phosphide counterpart of stishovite in the cosmochemically important Fe–Ni–P system: an indicator of significant shock events experienced by the iron and stony-iron meteorites or their parent bodies. The main obstacle to the application of this mineral as a high-pressure marker is its rarity, because until now, allabogdanite has only been identified in the three iron meteorites mentioned above. Concerning this issue, the discovery stories of allabogdanite in the Onello21 and the Santa Catharina meteorites (the present study) are curiously similar. In the Onello meteorite, the mineral was first described as barringerite46, the low-pressure polymorph of (Fe,Ni)2P31, on the basis of its chemical composition. However, the subsequent structural study of “barringerite” from the Onello meteorite resulted in the discovery of allabogdanite21. A similar situation occurred with the Santa Catharina mineral, which was formerly reported in this meteorite under the name “barringerite”42. The structural determination of “barringerite” from Santa Catharina performed in the present study revealed that this mineral is allabogdanite. It is noteworthy that the Santa Catharina meteorite was extensively studied for more than 30 years. The fact that allabogdanite has been overlooked in one of the best-studied iron meteorites suggests that this mineral might not be as rare as believed.

Among the reported occurrences of meteoritic (Fe,Ni)2P (refs31,52,53,54,55 and the works cited therein), only the first finding (the discovery) of barringerite, the low-pressure form of (Fe,Ni)2P, was supported by the X-ray diffraction data31. Herein, we showed that allabogdanite may frequently be misidentified as barringerite on the basis of only chemical (electron microprobe) data, leading to the eventual loss of important information related to the impact history of the studied meteorites. Fortunately, the two polymorphs of (Fe,Ni)2P, low-pressure barringerite and high-pressure allabogdanite, can be readily distinguished by the electron backscatter diffraction (EBSD) technique. The latter method, being non-destructive, very local and readily accessible, could facilitate the correct identification of allabogdanite, allowing us to record the impact history of meteorites, their parent bodies and possibly, the impact events that occurred on the Earth.

The occurrence of allabogdanite in nickel-rich ataxites opens new insights into the origin and space history of this meteorite group. The stability field of the high-pressure modification of (Fe,Ni)2P leads to two reliable scenarios of the formation of nickel-rich ataxites. The first scenario implies equilibrium crystallization of allabogdanite inside the Fe,Ni-metal-rich parts of a large celestial body under a pressure exceeding 8 GPa, which corresponds to the conditions of the Earth’s upper mantle at a depth greater than 250 km56. Subsequent fragmentation of the allabogdanite-bearing zone and quenching of the produced fragments could be accomplished through catastrophic collision of the allabogdanite parent body and the external impactor. In this case, nickel-rich ataxites represent examples of impact ejecta, which preserve information about the composition of the inner zone of their parent body.

The second scenario is consistent with the currently accepted formation scheme for the shocked (impact-veined) ordinary chondrites15,16,17,18,30. In this case, the primary precursor of allabogdanite was its low-pressure polymorph, barringerite31, which underwent crystal-to-crystal (topotactic) phase transformation22 during collision of the two metal-rich planetesimals. The pressure-temperature conditions of such impact events15,16,17,18 fall within the margins of the allabogdanite stability field. Besides the presence of allabogdanite, the studied meteorites exhibit common fracturing of the schreibersite-nickelphosphide crystals and brecciated structures of the troilite nodules (in the Santa Catharina meteorite), which supports the hypothesis of the experienced dynamic shock event.

From the authors’ point of view, the second scenario of the formation of nickel-rich ataxites seems more reliable because it does not require the existence of a large planetary body. However, some evidence, such as the crystallographically coincident growth of kamacite and taenite single crystals, as well as the diffusion-driven formation of the “cloudy zone” in the Barbianello meteorite (Fig. 2) argues for the long-time growth of the host Fe,Ni metal under equilibrium conditions5,6,8,9,57. It is important, however, that irrespective of the scenario realized, the Fe,Ni metal of the nickel-rich ataxites experienced rapid quenching in the solid state after the formation of allabogdanite, and was never reheated to a high temperature (800–1100 °C)22,25 upon the pressure release. Otherwise, in spite of known kinetic barriers of the allabogdanite-barringerite transition, the high-pressure form (allabogdanite) could not be preserved in the meteorite fragments. The latter means, in due course, that the cooling history of nickel-rich ataxites is principally different from the thermal history of the common magmatic groups of iron meteorites, which are known to have cooling rates of about 100–10000 °C/Myr2,9,57.


In the present study, we discovered allabogdanite, a high-pressure polymorph of (Fe,Ni)2P, in two iron meteorites, Santa Catharina and Barbianello. It is shown that allabogdanite is not a mineralogical curiosity and can be discovered in other meteorites upon detailed study. The mineral is routinely misidentified for its low-pressure analogue, barringerite, but can be readily distinguished from the latter using the non-destructive EBSD (electron backscatter diffraction) method. Allabogdanite, being the only known high-pressure mineral in the Fe–Ni–P system, can be used as a convenient stishovite-grade indicator of significant impact events experienced by the iron (and possibly other classes of) meteorites and their parent bodies.

Materials and Methods


Two specimens of the Santa Catharina meteorite (10 and 28 g weight) were obtained from the collection of Sergey Vasiliev (Prague, Czech Republic; The bar-like section of the Barbianello meteorite, 2 × 2 × 20 mm, was kindly loaned by R.P. from his collection. The specimen of the Onello iron, about 6 g weight, is the same one which has been described in the primary reference devoted to allabogdanite21.

Sample preparation

The specimens of the Santa Catharina and Onello meteorites were cut into a few slices; the specimen of the Barbianello meteorite was used as received. The cut sections were polished using conventional metallographic procedures and slightly etched with the nital etchant, in order to develop the phosphide inclusions.

Electron microprobe study

Electron microprobe analyses (EMPA) of phosphides and the metal were carried out using uncoated samples in energy dispersive mode (acceleration voltage 20 kV, beam current 2 nA), by means of a Hitachi S-3400N scanning electron microscope equipped with an Oxford Instruments AzTec Energy X-Max 20 spectrometer; acquisition time was set to 30 s per point. The following analytical standards were used: InP (PK), metallic Fe (FeK), Co (CoK) and Ni (NiK). No other elements with the atomic number greater than 4 were detected.

X-ray single crystal studies

The crystals of phosphides intended for the X-ray single crystal examination were extracted from the appropriate Santa Catharina sections after the local etching of the metal matrix in warm 15% HCl. Several crystal fragments of allabogdanite were extracted and checked with respect to suitability for the single-crystal study. The crystal #1 fragment (Fig. 1) was found to have the best quality. Single-crystal data were collected by means of a Bruker Kappa APEX DUO diffractometer equipped with a flat APEX II CCD detector, using MoKα radiation generated by the microfocus tube. Data collection was performed using Bruker Apex2 software58; subsequent data processing and integration routines were conducted using CrysAlis PRO program59. Crystal structure of allabogdanite from the Santa Catharina meteorite was solved and refined by means of a SHELX-2014 suite of programs60 embedded into Olex2 program package61. Supplementary Tables 1–3 and crystallographic information file (CIF) in the Supplementary Information contain the details of data collection, structure solution and refinement, atomic coordinates and thermal displacement parameters for allabogdanite from the Santa Catharina meteorite.

Electron backscatter diffraction (EBSD)

Polished sections suitable for the EBSD study were prepared using reactive ion etching (RIE) with Ar+ ions, by means of an Oxford Instruments IonFab-300 instrument operated at 500 V acceleration voltage and 2.4 mA/cm2 current density. EBSD measurements were carried out by means of a Hitachi S-3400N scanning electron microscope equipped with an Oxford Instruments Nordlys-HKL EBSD detector, operated at 20 kV and 1.5 nA in focused beam mode with a 70 ° tilted stage. The structures of the minerals were determined by matching the respective EBSD patterns with the reference structural models21,62,63.