Skip to main content
NCBI home page
ACS AuthorChoice logoLink to ACS AuthorChoice
. 2021 Sep 16;21(19):8135–8142. doi: 10.1021/acs.nanolett.1c02573

Discovery and Implications of Hidden Atomic-Scale Structure in a Metallic Meteorite

András Kovács †,*, Laura H Lewis ‡,#, Dhanalaksmi Palanisamy §, Thibaud Denneulin †, Alexander Schwedt ∥, Edward RD Scott ⊥, Baptiste Gault §,∇, Dierk Raabe §, Rafal E Dunin-Borkowski †, Michalis Charilaou @,*
PMCID: PMC8519181  PMID: 34529916

Abstract

graphic file with name nl1c02573_0006.jpg

Iron and its alloys have made modern civilization possible, with metallic meteorites providing one of the human’s earliest sources of usable iron as well as providing a window into our solar system’s billion-year history. Here highest-resolution tools reveal the existence of a previously hidden FeNi nanophase within the extremely slowly cooled metallic meteorite NWA 6259. This new nanophase exists alongside Ni-poor and Ni-rich nanoprecipitates within a matrix of tetrataenite, the uniaxial, chemically ordered form of FeNi. The ferromagnetic nature of the nanoprecipitates combined with the antiferromagnetic character of the FeNi nanophases gives rise to a complex magnetic state that evolves dramatically with temperature. These observations extend and possibly alter our understanding of celestial metallurgy, provide new knowledge concerning the archetypal Fe–Ni phase diagram and supply new information for the development of new types of sustainable, technologically critical high-energy magnets.

Keywords: magnetism, iron meteorite, tetrataenite, electron microscopy, tetragonal iron, micromagnetics

The study of ferrous meteorites informs our understanding of the solar system as well as of terrestrial metallurgy. These bodies, consisting primarily of iron and nickel, are remnants of protoplanetary cores that formed during the early solar system1−4 and are thought to have produced magnetic fields in a similar manner to Earth’s geodynamo.3 Although the original location of iron meteorites is thought to be the asteroid belt, that is, between the orbits of Mars and Jupiter, isotopic measurements suggest that some meteorites originated beyond Jupiter,5 while others came from the Earth-forming region in the interior of the solar system. Therefore, the study of metallic meteorites, which provide the oldest thermal and magnetic record of the early solar system, can provide a deep understanding of what may have been the precursor of Earth itself. From a materials science perspective, meteorites provide almost ideal environments for atomic arrangements to approach thermodynamic equilibrium during cooling over billions of years. Such conditions can permit the formation of tetrataenite (designation L10, AuCu-I prototype structure) which is extremely difficult to synthesize6,7 in macroscopic quantities suitable for technological applications. Tetrataenite’s alternating layers of Fe and Ni atoms are stacked parallel to the tetragonal c axis to form a superlattice that donates impressive technical magnetic properties.8 Tetrataenite is not documented in the conventional Fe–Ni binary phase diagram9 but may be found in meteoritical phase diagrams4,10−12 containing a complex set of ferromagnetic phases4,13,14 that are, by convention, designated by their Ni content. The L10 phase of FeNi forms during cooling from disordered face-centered cubic (fcc, designation A1) Ni-rich taenite. Other meteoritic phases include kamacite, the Ni-poor body-centered cubic (bcc, designation A2) alloy that contains a maximum of 5 atom % Ni,15−17 and awaruite, an intermetallic Ni3Fe-type compound with L12-type structure.11,18 These Fe–Ni phases and their crystallographic information are summarized in the Supporting Information. The kinetics of phase transformations in the Fe–Ni system are acknowledged to be extremely slow12 as a result of the sluggish interdiffusion of Fe and Ni, which is likely influenced by magnetic long-range order.2 Details of the phase assemblage in a meteorite determine its internal magnetic field,19,20 which impacts the interpretation of its thermal history.2,18

The current understanding of meteoritic magnetism relies on the interpretation of the microstructure, but considering the complexity of the Fe–Ni phase diagram and the varying cooling conditions over billions of years, it is possible for nonequilibrium nanoscopic phases to be stabilized in a meteorite that have an effect on the overall magnetic state. Here, we report for the first time the observation of an exotic Ni-poor tetragonal phase with an antiferromagnetic state.

A Clandestine Meteoritic Microstructure

In this work, the investigation was focused on the NWA 6259 meteorite which consists of a very large multivariant region of tetrataenite6 and possesses the second highest Ni content (∼43 atom %) of all reported meteorites. The structure of the NWA 6259 specimen is shown on different length scales in Figure 1. Details of sample preparation and characterization techniques are provided in the Supporting Information (Figure S3). A sample for study was removed from the central region of the meteorite specimen (Figure 1a) and was determined to possess an approximate mesoscopic composition of Fe 57 atom % and Ni 43 atom %; with Co (∼3 atom %) and a minor enrichment in Cu; the dark inclusions observed in Figure 1a contain sulfur and phosphorus. The information on Cu precipitates can be found in the Supporting Information (Figure S4). A crystallographic orientation map derived from electron backscatter diffraction (EBSD) data (Figure 1a) reveals that, within the resolution limit of the technique, this region can be considered as a single crystal. This orientation map guided the preparation of crystallographically defined electron-transparent specimens (Figure 1b) for higher resolution studies. The regular pattern observed within the meteorite structure (Figure 1b) resembles the well-known Widmanstätten structure;2 however, the results reveal that the structure below is not composed of taenite and kamacite phases. The specimen matrix contains a network of precipitates and lamellar inclusions (Figures 1b,c) and is verified to possess tetragonal symmetry with superlattice diffraction reflections (Figure 1d) that signal the long-range chemical order of L10 FeNi, tetrataenite. The high degree of chemical order of the tetrataenite matrix is confirmed by the small but finite intensity difference attributed to alternate scattering of Fe and Ni atom columns detected by high-angle annular dark field (HAADF) scanning transmission electron microscopy (TEM) (Figure 1e).

Figure 1.

Figure 1

Open in a new tab

Microstructure of meteorite NWA 6259. (a) Electron backscatter diffraction image quality map recorded from the fragment used for electron microscopy. The dark gray inclusions contain sulfur and phosphorus. The inverse pole figure map with respect to the sample normal direction on the right shows that the crystal is one grain. (b) Bright-field TEM image showing lamellar microstructure. (c) Magnified bright-field TEM image revealing precipitates adjacent to lamellae in the Fe–Ni matrix. (d) Electron diffraction pattern recorded from the area shown in panel b, consistent with an ordered tetragonal L10 structure. The viewing direction is [110]. Red triangles mark superlattice reflections. (e) HAADF STEM image of the tetrataenite L10 FeNi matrix. The enlarged region and schematic diagram on the right shows a primitive unit cell of the tetragonal phase. Intensity variations in the line profile, which was obtained from the marked region, are associated with differences in atomic number Z between Fe (Z = 26) and Ni (Z = 28). The detector semiangle used was 69 mrad.

The structure and composition of small (Figure 1c) crystalline precipitates within the L10 matrix were examined at Ångstrom-level resolution using correlative electron microscopy and 3-dimensional (3D) atom probe tomography (APT) performed on the needle-shaped specimen (Figure 2a) prepared using focused ion beam (FIB) milling. These results confirm the tetrataenite composition itself as 45 atom % Ni/55 atom % within the matrix; iso-composition surfaces superimposed onto the reconstructed tomographic 3D point cloud reveal that regions richer than 26 atom % Ni (Figure 2b) contain a dense distribution of Ni-poor (∼90 atom % Fe) precipitates with a bimodal distribution of coarse (28 ± 6 nm) and ultrafine (2.0 ± 0.5 nm) average diameters at approximately 15 000 precipitates per cubic micrometer (Figure 3). The 50 atom % iso-composition level reveals Ni-rich lamellae of composition of ∼66 atom % Ni, close to that of the ideal composition of the awaruite,11,21Figure 2c. A combined tomographic reconstruction in Figure 2c shows the overall nanostructure, together with corresponding quantitative elemental composition scans.

Figure 2.

Figure 2

Open in a new tab

Fe–Ni phase decomposition in the tetrataenite matrix. (a) Bright-field TEM image of a needle-shaped specimen prepared for atom probe tomography reconstruction. The marked region (red cone) is reconstructed and analyzed in panel b. (b) Reconstruction showing Ni-poor (Fe-rich) regions (red) delineated by 26 atom % Ni iso-concentration surfaces. The corresponding elemental concentration profiles (I and II) across the particles marked in panel b (Fe, red; Ni, green), showing an Fe composition close to 90 atom %. (c) Reconstruction of the precipitates and lamella delineated by a 50 atom % Ni iso-concentration surface. On the basis of the Fe–Ni phase diagram, the lamella is inferred to be awaruite, fcc FeNi2. The corresponding composition profile along the line marked in panel c shows Fe and Ni enrichment in the tetrataenite matrix.

Figure 3.

Figure 3

Open in a new tab

Structure and strain analyses. (a) Overview HAADF STEM image of a bcc A2 Fe–Ni precipitate (25 nm × 35 nm), shown alongside (b) an atomic-resolution HAADF STEM image of the A2/L10 interface, which is decorated by misfit dislocations every 1–2 nm. The inset Fourier transforms confirm the bcc structure of the precipitate. (c) Overview bright-field STEM image of ultrafine (<5 nm) Ni-poor A6 Fe–Ni precipitates (dark). (d) Atomic-resolution HAADF STEM image of an A6 precipitate next to a three-monolayers-thick Ni-rich L12 lamella. (e) Strain rotation map of the A6 and L12 lamella shown in panel d. Arrows mark misfit dislocations at the precipitate boundary. (f) Strain and shear in the region marked in panel e across the A6 precipitate and L12 lamella.

Nanostructure, Strain, and a New Fe–Ni Phase

A fascinating aspect of the meteorite nanostructure is the role that strain plays in the crystallographic features of two types of Ni-poor precipitates embedded within the L10-type matrix. A representative coarse Ni-poor precipitate, embedded incoherently in the matrix, is delineated by regularly spaced (1–2 nm) misfit dislocations at the precipitate–matrix interface ([100]A2(010)A2∥[110]L10(001)L10 orientational relationship) and is confirmed to adopt the bcc (A2-type) structure (Figure 3a,b). In contrast, the ultrafine (1–2 nm) Ni-poor precipitates, Figure 3c,d, coherently embedded in the matrix, have the same crystal symmetry as the surrounding L10 matrix but possess a chemically disordered face-centered tetragonal (A6-type) crystal structure with unit cell parameters similar to tetrataenite. These ultrafine precipitates are lattice-matched to the tetrataenite matrix but possess a composition of 90 atom % Fe. To the best of our knowledge, this is the first report of a tetragonal Ni-poor phase in the Fe–Ni system, although recently the synthesis of tetragonal, nominally equiatomic FeNi has been confirmed.8,22

A relatively big, 4 nm-diameter Ni-poor precipitate, adjacent to a Ni-rich lamella, Figure 3d, is characterized by a strain field as revealed by geometric phase analysis based on Fourier transformation of a high-resolution STEM image as shown in Figure 3e,f. This region, which contains two dislocations and a corresponding strain at the phase boundary (Figure 3e), is consistent with the interpretation of nanoscale decomposition of the metastable tetrataenite phase through precipitation of Ni-poor phases with either cubic A2 (coarse kamacite precipitates) or tetragonal A6 (utrafine precipitates) crystal structures and a lamellar Ni-rich L12-type phase. While the two types of Ni-poor precipitates are nearly isotropic in shape and are distributed evenly in the matrix, the Ni-rich awaruite precipitates follow distinct crystallographic directions in the matrix, suggesting that Ni migrated along diffusion-favorable directions to form the lamellae, leaving behind Ni-poor pockets.

The tetragonal A6-structured FeNi phase in this meteorite divulges a fascinating new aspect of the Fe–Ni system. The close relationship between various cubic symmetries was formalized long ago as the Bain distortion,23 in which a bcc lattice can be obtained from an fcc lattice by a compression parallel to the c axis and an expansion along an a axis to form a body-centered tetragonal lattice.24 The A6 structure adopted by the ultrafine Ni-poor precipitates is likely stabilized through largely coherent bonding to the parent tetragonal L10 phase. These ultrafine A6 precipitates can be considered as Guinier-Preston (G.P.) zones, which are manifestations of an initial stage of precipitation during solid-state phase decomposition.25 G.P. zones typically possess an intermediate crystal structure and composition that are different from those of both the thermodynamically stable phase and the host phase.

Effects of Phase Diversities on Magnetic Properties

The presence and diversity of these Fe–Ni phases impacts both the micromagnetic and bulk magnetic states of the material, and consequently influences how magnetometry is used to interpret meteoritic history as well as to evaluate tetrataenite’s potential as a technological material. The results reported here confirm that the NWA 6259 meteorite, and therefore likely other stony, stony-iron, and iron meteorites, can be regarded as magnetic nanocomposites with strong interphase magnetic coupling. Magnetic configurations in nanocomposites have been studied extensively as novel exchanged-coupled permanent magnets,19,26 and it is known that extrinsic, or technical, magnetic properties such as coercivity and remanence depend on the volume fractions of the phases, the diameters of precipitates and the degree of exchange coupling at interfaces. To investigate these aspects, the magnetic configuration of the NWA 6259 meteorite was studied using Lorentz TEM and off-axis electron holography27 (Figures 4a–d) applied to the same samples that were investigated using microstructural characterization. The details of the magnetic phase shift measurements can be found in the Supporting Information (Figure S5). Magnetic imaging in the remanent state was conducted in specimens prepared with the magnetic easy axis of the L10 FeNi phase oriented both in-plane (Figures 4a,b) and out-of-plane (Figures 4c,d). These images reveal a high density of 180° or 90° magnetic domains, with sizes ranging from 100 to 500 nm. Quantitative magnetic induction maps (Figures 4b,d) indicate that the 180° magnetic domain walls are almost parallel to the magnetic easy axis, as expected for a uniaxial system.28 The magnetic domain walls are distorted in the vicinity of the Ni-rich lamellae, marked by dashed lines. This distortion is attributed to the difference in the magnetocrystalline anisotropy energy of the L10 and L12 Fe–Ni phases. The Ni-poor A2 nano- and A6 ultrafine precipitates are not observed to affect the overall magnetic domain configuration in the studied samples. Nonetheless, all phases impact the magnetic state, and the nature of the A6-type (tetragonal) precipitates is of particular interest. Computational29,30 and experimental31,32 investigations of fcc-type iron indicate an antiferromagnetic33−36 (AFM) ground state that is typically not accessible because the A2 (bcc) to A1 (fcc) phase transition in iron occurs above its Curie temperature (i.e., the temperature below which it is ferromagnetic). An atomistic simulation of a noncollinear configuration of atomic moments leads to zero net magnetization (Figure S6). As AFM ordering breaks cubic symmetry, antiferromagnetism is intimately linked to the presence of a structural distortion.37−39 Thus, the A6-type tetragonal Fe(Ni) phase stabilized in the NWA 6259 meteorite is anticipated to exhibit antiferromagnetism. The existence of a transient antiferromagnetic phase in the NWA 6259 meteorite was confirmed with bulk thermomagnetic measurements conducted in a low magnetic field on a single sample of the as-received NWA 6259 meteorite. Two consecutive heating and cooling cycles in the temperature range 300 K ≤ T ≤ 900 K (Figure 4e) were performed, with a full magnetic hysteresis loop measured at room temperature before and after each thermal excursion (Figure 4f). The first heating branch confirmed the reported tetrataenite kinetic Curie temperature TC1 ∼ 830 K.6,12 Upon the first cooling, the magnetization remained close to zero until an apparent second Curie temperature of TC2 ∼ 740 K where it rose to a value of 65 kA/m that was maintained down to room temperature (Figure 4f). The corresponding hysteresis loop returned a room temperature saturation magnetization of 1150 kA/m, same as that of the as-received state, but with a vanishingly small coercivity much decreased from the as-received value of 0.1 T, as expected for the chemically disordered FeNi phase. The low-field magnetization of the second heating cycle dipped slightly at ∼660 K and then fell abruptly at TC2 ∼ 740 K. Upon the final cooling from 900 K, the magnetization again remained at an extremely low value down to a new magnetic transition at TC3 ∼ 660 K to rise again to 65 kA/m. Most strikingly, the final hysteresis loop indicated a 14% increase of the room temperature saturation magnetization to ∼1260 kA/m (Figure 4f) with coercivity still at nearly zero. These results motivated an in situ annealing study in the TEM (Figure 4g), which indicates that dissolution of the noted precipitates and concurrent disordering of the L10 structure begins at T ∼ 600 K after approximately 1 h. No clear sign of precipitates nor of L10 superlattice reflections were detectable at 923 K and after cooling the specimen to room temperature (Supporting Information, Figure S7). Overall, these results are consistent with the existence of a transitional phase with a magnetic transition temperature of 740 K that bridges the chemically ordered L10 FeNi phase and the disordered A1-type FeNi phase22 of Curie temperature 660 K. This study also demonstrates that, upon heating, the large population of Ni-rich and Ni-poor precipitates dissolve into the tetrataenite matrix, which itself undergoes chemical disordering. These changes combine to collapse the magnetocrystalline anisotropy and yield magnetically soft behavior. Finally, the large increase in saturation magnetization noted in the third and final room temperature hysteresis loop is consistent with dissolution of the A6-type AFM ultrafine phase, which was previously providing magnetic voids that reduced the matrix saturation magnetization of the meteorite.

Figure 4.

Figure 4

Open in a new tab

Magnetic properties of NWA 6259. (a) Fresnel defocus image of a specimen in which the magnetic easy axis ([001] of L10, c axis) is in-plane. Bands of black and white contrast arise from the presence of magnetic domain walls. Variations in contrast marked with yellow triangles suggest local changes in wall inclination. (b) Magnetic induction map measured using off-axis electron holography from the dashed region in panel a, showing 180° magnetic domain walls. Dashed lines mark the locations of Ni-rich lamella precipitates. Colors and arrows indicate the magnetic field direction. Contour spacing: 2π radians. (c) Fresnel defocus image of a specimen in which the magnetic easy axis is out-of-plane. Defocus: 0.5 mm. (d) Magnetic induction map showing a complex arrangement of magnetic domains. Contour spacing: 2π radians. (e) Thermomagnetic curves M(T) 1 and M(T) 2. The ferromagnetic transition temperature is 830 K. (f) Magnetization hysteresis curves measured in the “as received” condition and after annealing cycles (M(T) 1, 2). (g) Precipitate dissolution and chemical disordering observed in bright-field TEM images and SAED patterns recorded at 373, 773, and 923 K. Red triangles mark 001 reflections of the ordered L10 structure.

This conceptualized micromagnetic state was simulated with a model (Figure 5) based on the microstructure derived from the imaging data of the NWA 6259 specimen (Figure 1), including the number density and type of precipitates determined from the APT experiments (Figure 2). The ferromagnetic A2-type cubic precipitates were distributed evenly and randomly throughout the sample, whereas the A6-type AFM nanoprecipitates were simulated as nonmagnetic 2 nm-diameter voids with a vanishing magnetization. The resultant contour plot of the magnetization component parallel to the L10c axis (easy axis), Figure 5c, shows a simulated micromagnetic domain state with 180° magnetic domains parallel to the c axis with widths of approximately 200 nm that is in excellent agreement with the experiment (Figure 4b). Closer inspection of the simulated domain walls reveals a straight wall structure (Figure 5d) and distortions, or kinks, at intersections with L12 lamellae (Figure 5e), exactly as found in the electron microscopy experiment (Figure 4b). A detailed view of the local magnetization rotation and Bloch domain wall broadening at a phase intersection is shown in Figure 5e. These kinks are attributed to the difference in magnetic anisotropy, and consequently in the magnetic domain wall energy and width, between the L10 and L12 phases. The magnetic domain wall width is calculated as 5.6 nm in the L10 phase and 18 nm in the L12 phase (Supporting Information, Figure S6b). Further, Figure 5e shows how the chirality of the domain wall differs on either side of the L12 lamella, a feature associated with minimization of the dipole–dipole energy state of the domain wall that has implications for the stability of the ensemble magnetic state. These domain walls signal magnetically weak spots where magnetization curling instabilities can form and facilitate magnetization reversal.

Figure 5.

Figure 5

Open in a new tab

Micromagnetic simulations of A2, A6, and L12 Fe–Ni precipitates in an L10 FeNi matrix. (a) Simulation system based on the TEM image of the NWA 6259 specimen shown in Figure 1e. (b) 3D visualization of the simulated structure, showing randomly distributed spheroidal A2 and A6 Fe–Ni precipitates. (c) Simulation of an equilibrium magnetic state with domain walls parallel to the c axis of the L10 structure. (d,e) Simulations showing that a domain wall that propagates through an L12 lamella is bent. An example is marked by a white rectangle. Magnified view showing twisting of the local magnetization at the intersection with the L12 lamella.

Scientific and Technological Implications of the Meteoritic Hidden Microstructure

New knowledge of the previously undescribed “hidden” structure and properties of the NWA 6259 meteorite reported here impacts not only how iron meteoritic data might be used to interpret the origins of our solar system but also invites renewed consideration of tetrataenite as a sustainable permanent magnet. Utilizing highest-resolution probes combined with magnetometry and simulations, the microstructure is revealed to comprise a magnetic phase assemblage of ferromagnetic cubic (∼30 nm diameter), antiferromagnetic tetragonal (∼2 nm diameter) precipitates and ferromagnetic L12-type lamellae embedded in a tetrataenite matrix. At the current time these antiferromagnetic precipitates are not considered to be the hypothesized antitaenite phase,40−42 on the basis of different postulated formation modes, crystal structures, and magnetic transition temperatures. These antiferromagnetic precipitates decrease the saturation magnetization and the soft magnetic inclusions act as weak regions that nucleate easy magnetization reversal. Both of these effects decrease the technical magnetic properties of the meteoritic sample, advancing the deduction that the maximum energy product of tetrataenite, deduced from measurements of natural materials such as the NWA 6259 meteorite, may be underestimated by as much as 15–20% to reach a value that is close to 70% of that of the best rare-earth magnets showing promise for closing the performance gap of permanent magnets.43 This conclusion invites renewed consideration of tetrataenite as a sustainable advanced permanent magnet.

Acknowledgments

The authors are grateful to L. Kibkalo, D. Meertens, and W. Pieper for TEM specimen preparation and to M. Keil for EBSD preparation. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant No. 856538, project “3D MAGiC”) and from the Horizon 2020 Research and Innovation Programme (Grant No. 823717, project “ESTEEM3”). Funding by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) via CRC/TRR 270 “HoMMage” (Project-ID 405553726) is gratefully acknowledged. Portions of this research were conducted with high performance computational resources provided by the Louisiana Optical Network Infrastructure (http://www.loni.org). This research was supported in part by a cooperative agreement with U.S. Department of Energy’s Advanced Research Projects Agency-Energy (ARPA-E) and by Northeastern University.

Supporting Information Available

The Supporting Information is available free of charge at https://pubs.acs.org/doi/10.1021/acs.nanolett.1c02573.

  • Mechanical preparation of NWA 6259 meteorite; focused ion beam specimen preparation and transmission electron microscopy methods; basic structure information on Fe–Ni phases; unit cell determination in L10 FeNi; acquisition and reconstruction of electron phase shift images by off-axis electron holography; details of micromagnetic simulations; pole figure and composition analysis of the bulk sample; atom-probe tomography measurement and analysis of Cu precipitates; bimodal size distribution of A6 and A2-type precipitates; atomistic spin dynamics simulation of fcc Fe; magnetic domain wall profiles in L10 and L12 phases; in situ TEM annealing (PDF)

The authors declare no competing financial interest.

Supplementary Material

nl1c02573_si_001.pdf (13.6MB, pdf)

References

  1. Krot A. N.; Keil K.; Scott E. R. D.; Goodrich C. A.; Weisberg M. K. In Meteorites, Comets and Planets, Treatise on Geochemistry Update 1; Davis A., Ed.; Elsevier: Amsterdam, 2008; Chapter Classification of meteorites, pp 1–63. [Google Scholar]
  2. Goldstein J. I.; Scott E. R. D.; Chabot N. L. Iron meteorites: crystallization, thermal history, parent bodies, and origin. Chem. Erde 2009, 69, 293–325. 10.1016/j.chemer.2009.01.002. [DOI] [Google Scholar]
  3. Weiss B. P.; Elkins-Tanton L. T. Differentiated planetesimals and the parent bodies of chondrites. Annu. Rev. Earth Planet. Sci. 2013, 41, 529–560. 10.1146/annurev-earth-040610-133520. [DOI] [Google Scholar]
  4. Scott E. R. D. Iron Meteorites: Composition, Age, and Origin. Oxford Research Encyclopedias, Planetary Science 2020, 1, 1–75. 10.1093/acrefore/9780190647926.013.206. [DOI] [Google Scholar]
  5. Kruijer T. S.; Burkhardt C.; Budde G.; Kleine T. Age of Jupiter inferred from the distinct genetics and formation times of meteorites. Proc. Natl. Acad. Sci. U. S. A. 2017, 114, 6712–6716. 10.1073/pnas.1704461114. [DOI] [PMC free article] [PubMed] [Google Scholar]
  6. Poirier E.; Pinkerton F. E.; Kubic R. C.; Mishra R.; Bordeaux N.; Mubarok A.; Lewis L. H.; Goldstein J. I.; Skomski R.; Barmak K. Intrinsic magnetic properties of L10 FeNi obtained from meteorite NWA 6259. J. Appl. Phys. 2015, 117, 17E318. 10.1063/1.4916190. [DOI] [Google Scholar]
  7. Lewis L. H.; Mubarok A.; Poirier E.; Bordeaux N.; Manchanda P.; Kashyap A.; Skomski R.; Goldstein J.; Pinkerton F. E.; Mishra R. K.; Jr R. C. K.; Barmak K. Inspired by nature: investigating tetrataenite for permanent magnet applications. J. Phys.: Condens. Matter 2014, 26, 064213. 10.1088/0953-8984/26/6/064213. [DOI] [PubMed] [Google Scholar]
  8. Maat N.; McDonald I.; Barua R.; Lejeune B.; Zhang X.; Stephen G. M.; Fisher A.; Heiman D.; Soldatov I. V.; Schäfer R.; Lewis L. H. Creating, probing and confirming tetragonality in bulk FeNi alloys. Acta Mater. 2020, 196, 776–789. 10.1016/j.actamat.2020.07.019. [DOI] [Google Scholar]
  9. Swartzendruber L. J.; Itkin V. P.; Alcock C. B. The Fe-Ni (iron-nickel) system. J. Phase Equilib. 1991, 12, 288. 10.1007/BF02649918. [DOI] [Google Scholar]
  10. Yang C. W.; Williams D. B.; Goldstein J. I. A revision of the Fe-Ni phase diagram at low temperatures (< 400 °C). J. Phase Equilib. 1996, 17, 522. 10.1007/BF02665999. [DOI] [Google Scholar]
  11. Howald R. A. The thermodynamics of tetrataenite and awaruite: a review of the Fe–Ni phase diagram. Metall. Mater. Trans. A 2003, 34A, 1759–1769. 10.1007/s11661-003-0142-9. [DOI] [Google Scholar]
  12. Dos Santos E.; Gattacceca J.; Rochette P.; Fillion G.; Scorzelli R.B. Kinetics of tetrataenite disordering. J. Magn. Magn. Mater. 2015, 375, 234–241. 10.1016/j.jmmm.2014.09.051. [DOI] [Google Scholar]
  13. Scott E. R. D. The nature of dark-etching rims in meteoritic taenite. Geochim. Cosmochim. Acta 1973, 37, 2283–2294. 10.1016/0016-7037(73)90104-X. [DOI] [Google Scholar]
  14. Yang J.; Goldstein J. I.; Scott E. R. D. Iron meteorite evidence for early formation and catastrophic disruption of protoplanets. Nature 2007, 446, 888. 10.1038/nature05735. [DOI] [PubMed] [Google Scholar]
  15. Owen E. A.; Burns B. D. X-ray study of some meteoritic irons. Philos. Mag. 1939, 28, 497. 10.1080/14786443908521237. [DOI] [Google Scholar]
  16. Clarke R. S.; Goldstein J. I.. Smithsonian Contributions fo the Earth Sciences; Smithsonian Institution Press: Washington DC., 1978; Chapter Schreibersite growth and its influence on the metallography of coarse-structured iron meteorites, pp 1–83. [Google Scholar]
  17. Yang J.; Goldstein J. I. The formation of the Widmanstätten structure in iron meteorites. Meteor. Planet. Sci. 2005, 40, 239–253. 10.1111/j.1945-5100.2005.tb00378.x. [DOI] [Google Scholar]
  18. Yang C. W.; Williams D. B.; Goldstein J. I. Low-temperature phase decomposition in metal from iron, stony-iron, and stony meteorites. Geochim. Cosmochim. Acta 1997, 61, 2943–2956. 10.1016/S0016-7037(97)00132-4. [DOI] [Google Scholar]
  19. Skomski R.; Manchanda P.; Kumar P. K.; Balamurugan B.; Kashyap A.; Sellmyer D. Predicting the future of permanent-magnet materials. IEEE Trans. Magn. 2013, 49, 3215–3220. 10.1109/TMAG.2013.2248139. [DOI] [Google Scholar]
  20. Einsle J. F.; Eggeman A. S.; Martineau B. H.; Saghi Z.; Collins S. M.; Blukis R.; Bagot P. A. J.; Midgley P. A.; Harrison R. J. Nanomagnetic properties of the meteorite cloudy zone. Proc. Natl. Acad. Sci. U. S. A. 2018, 115, E11436–E11445. 10.1073/pnas.1809378115. [DOI] [PMC free article] [PubMed] [Google Scholar]
  21. Wakelin R. J.; Yates E. L. A study of the order-disorder transformation in iron-nickel alloys in the region FeNi3. Proc. Phys. Soc., London, Sect. B 1953, 66, 221–240. 10.1088/0370-1301/66/3/310. [DOI] [Google Scholar]
  22. Montes-Arango A.M.; Marshall L.G.; Fortes A.D.; Bordeaux N.C.; Langridge S.; Barmak K.; Lewis L.H. Discovery of process-induced tetragonality in equiatomic ferromagnetic FeNi. Acta Mater. 2016, 116, 263–269. 10.1016/j.actamat.2016.06.050. [DOI] [Google Scholar]
  23. Bain E. C. The nature of martensite. Trans. AIME 1924, 70, 25. [Google Scholar]
  24. Bowles J. S.; Wayman C. M. The bain strain, lattice correspondences, and deformations related to martensitic transformations. Metall. Trans. A 1972, 3, 1113. 10.1007/BF02642442. [DOI] [Google Scholar]
  25. Abbaschian R.; Abbaschian L.; Reed-Hill R. E.. Physical Metallurgy Principles; Von Notstrand: New York, 2009; pp 504–506. [Google Scholar]
  26. Skomski R. J. Phys.: Condens. Matter 2003, 15, R841. 10.1088/0953-8984/15/20/202. [DOI] [Google Scholar]
  27. Kovács A.; Dunin-Borkowski R. E. In Handbook of Magnetic Materials; Brück E., Ed.; Elsevier: 2018; Vol. 27, pp 59–153. [Google Scholar]
  28. Kittel C. Physical theory of ferromagnetic domains. Rev. Mod. Phys. 1949, 21, 541–583. 10.1103/RevModPhys.21.541. [DOI] [Google Scholar]
  29. Pinski F. J.; Staunton J.; Gyorffy B. L.; Johnson D. D.; Stocks G. M. Ferromagnetism versus antiferromagnetism in face-centered-cubic iron. Phys. Rev. Lett. 1986, 56, 2096–2099. 10.1103/PhysRevLett.56.2096. [DOI] [PubMed] [Google Scholar]
  30. Moruzzi V. L.; Marcus P. M.; Kübler J. Magnetovolume instabilities and ferromagnetism versus antiferromagnetism in bulk fcc iron and manganese. Phys. Rev. B: Condens. Matter Mater. Phys. 1989, 39, 6957–6961. 10.1103/PhysRevB.39.6957. [DOI] [PubMed] [Google Scholar]
  31. Tsunoda Y.; Kunitomi N. Structural phase transition of γ-Fe precipitates in Cu. J. Phys. F: Met. Phys. 1988, 18, 1405. 10.1088/0305-4608/18/7/010. [DOI] [Google Scholar]
  32. Tsunoda Y; Imada S; Kunitomi N Anomalous lattice contraction and magnetism of γ-Fe precipitates in Cu. J. Phys. F: Met. Phys. 1988, 18, 1421. 10.1088/0305-4608/18/7/011. [DOI] [Google Scholar]
  33. Lavrentiev M. Y.; Wrobel J. S.; Nguyen-Manh D.; Dudarev S. L. Magnetic and thermodynamic properties of face-centered cubic Fe-Ni alloys. Phys. Chem. Chem. Phys. 2014, 16, 16049. 10.1039/C4CP01366B. [DOI] [PubMed] [Google Scholar]
  34. Abrikosov I. A.; Kissavos A. E.; Liot F.; Alling B.; Simak S. I.; Peil O.; Ruban A. V. Competition between magnetic structures in the Fe rich fcc FeNi alloys. Phys. Rev. B: Condens. Matter Mater. Phys. 2007, 76, 014434. 10.1103/PhysRevB.76.014434. [DOI] [Google Scholar]
  35. Xiong W.; Zhang H.; Vitos L.; Selleby M. Magnetic phase diagram of the Fe-Ni system. Acta Mater. 2011, 59, 521–530. 10.1016/j.actamat.2010.09.055. [DOI] [Google Scholar]
  36. Sjöstedt E.; Nordström L. Noncollinear full-potential studies of γ-Fe. Phys. Rev. B: Condens. Matter Mater. Phys. 2002, 66, 014447. 10.1103/PhysRevB.66.014447. [DOI] [Google Scholar]
  37. Marsman M.; Hafner J. Broken symmetries in the crystalline and magnetic structures of γ-iron. Phys. Rev. B: Condens. Matter Mater. Phys. 2002, 66, 224409. 10.1103/PhysRevB.66.224409. [DOI] [Google Scholar]
  38. Massalski T. B.; Laughlin D. E. The surprising role of magnetism on the phase stability of Fe (Ferro). CALPHAD: Comput. Coupling Phase Diagrams Thermochem. 2009, 33, 3. 10.1016/j.calphad.2008.07.009. [DOI] [Google Scholar]
  39. Lloyd S. J.; Dunin-Borkowski R. E. Electronic structure of face-centered-tetragonal iron in ferromagnetic iron-copper multilayers. Phys. Rev. B: Condens. Matter Mater. Phys. 1999, 59, 2352–2362. 10.1103/PhysRevB.59.2352. [DOI] [Google Scholar]
  40. Rancourt D.; Scorzelli R. Low-spin γ-Fe-Ni (γLS) proposed as a new mineral in Fe-Ni-bearing meteorites: epitaxial intergrowth of γLS and tetrataenite as a possible equilibrium state at ∼ 20–40 at% Ni. J. Magn. Magn. Mater. 1995, 150, 30–36. 10.1016/0304-8853(95)00089-5. [DOI] [Google Scholar]
  41. Rancourt D.; Scorzelli R. Low-spin γLS,-Fe-Ni proposed as a new meteoritic mineral - Reply. J. Magn. Magn. Mater. 1997, 174, 324–330. 10.1016/S0304-8853(97)00258-8. [DOI] [Google Scholar]
  42. Rancourt D.; Lagarec K.; Densmore A.; Dunlap R.; Goldstein J.; Reisener R.; Scorzelli R. Experimental proof of the distinct electronic structure of a new meteoritic Fe - Ni alloy phase. J. Magn. Magn. Mater. 1999, 191, L255–L260. 10.1016/S0304-8853(98)00366-7. [DOI] [Google Scholar]
  43. Coey J. Permanent magnets: Plugging the gap. Scr. Mater. 2012, 67, 524–529. 10.1016/j.scriptamat.2012.04.036. [DOI] [Google Scholar]

Associated Data

This section collects any data citations, data availability statements, or supplementary materials included in this article.

Supplementary Materials

nl1c02573_si_001.pdf (13.6MB, pdf)

Articles from Nano Letters are provided here courtesy of American Chemical Society

RESOURCES