Meteoritic Origin Research Articles

Methods for determination of the source of iron in precontact Inuit and Dorset culture artifacts from the Canadian Arctic

The period during which Dorset Culture peoples and precontact Inuit used iron was widespread and overlapped the appearance of the Norse in Greenland. In Greenland and Arctic Canada, three sources of iron in artifacts have been reported: terrestrial native iron, Norse wrought iron and meteoritic iron from the Cape York iron meteorite. We investigated the source of iron from fourteen samples of iron artifacts recovered from one precontact Inuit and three Dorset culture sites. Polished mm-scale samples mounted in polyester resin blocks yielding a roughly rectangular 1 × 2 mm cross section to preserve as much of each sample as possible were examined. Petrographic examinations by reflected light microscopy and SEM observation coupled with energy-dispersive analysis revealed the presence of Widmanstätten structure (an intergrowth of kamacite and taenite), a suite of minerals comprising kamacite, taenite, daubreelite and schreibersite and nickel-content at iron meteorite levels indicating all fourteen samples were unambiguously of meteoritic origin. With the meteoritic origin confirmed, Goldstein’s (1965) model relating half-width of the kamacite lamellae in the Widmanstätten patterns to the Ni-content of the lamellae was used to determine whether the meteoritic iron originated from the Cape York meteorite. A test of the method used the mean kamacite bandwidth and the bulk Ni-content of the Cape York mass Savik I, which demonstrated the validity of the basis of the method. Using the experimentally-derived relation between kamacite half-width of the bands and composition of the kamacite, the nickel-content of the kamacite lamellae ranged from 6.13 to 6.61 wt% Ni. These compositions are consistent with bandwidths that are narrower than the mean for Cape York, the anticipated source. The discrepancy may be attributed to flattening of the kamacite lamellae by cold working in the manufacture of the artifacts. As well, it has been shown that a range of bandwidths is typical in large iron meteorites such as Cape York. Thus, this method cannot definitively identify Cape York as the source of the meteoritic iron in the fourteen samples; however, the results can serve to identify meteoritic artifacts if the material that has not been intensively cold worked and if sufficient bandwidths can be measured in order to establish a mean thickness.

Patterns of groundwater chemistry: implications of groundwater flow and the relation with groundwater fluoride contamination in the phreatic aquifer of Odisha, India

The work analyzes the patterns of quality parameters and hydrochemical facies of 1105 nos (n = 685 in hard rock; n = 420 in alluvium) of groundwater samples drawn from the phreatic aquifer in Odisha, India. The study explores the possible relations of the groundwater chemistry including the fluoride (Fˉ) contaminations with the flow mechanisms. The hydrochemical facies types of Na-Mg-Ca-Cl-HCO3 characterize the groundwater discharge corridors lying close to the river valleys, and in parts of coastal alluvium, particularly in the Mahanadi deltaic region. In contrast, the facies types of Ca-Mg-HCO3-Cl dominate the groundwater recharge areas, located at relatively higher elevations. The recharge areas in the state are largely free from groundwater Fˉ contamination. The study delineates the ratio of Ca2+/Na+ and its distribution patterns to interpret the source of Fˉ (> 1.0 mg/L) in groundwater. The Ca2+/Na+ ratios of 1.0 are characterized by water types like Ca-Mg-HCO3 (Cl) of recent meteoritic origin. These are distributed in the groundwater recharge-midline areas where significant infiltration to groundwater occurs. The largest such cluster is observed in the Hirakud Canal Command area in the western parts of the state, indicating the role of anthropogenic sources of groundwater Fˉ contamination through irrigation return flows.

Fluid geochemistry in a low-enthalpy geothermal field along a sector of southern Apennines chain (Italy)

The chemical and isotopic features of the fluids (water and gases) in the Lucane thermal area (southern Italy) have been investigated in order to verify their origin, water temperature in the geothermal reservoir, and to recognize the main natural processes concerning the water composition during ascent towards the surface. The Lucane geothermal system is placed in the southern sector of the Apennines chains, a seismically active area, close to the southern base of the Mt. Alpi carbonate massif. Along the study area, two main sets of high-angle faults form an almost orthogonal fault system that, as suggested by local structural geology, acts as a preferential pathway for uprising deep fluids. Here, we recognized two different types of waters: (i) cold shallow waters having a meteoritic origin and interacting with carbonate rocks (dolomite and calcite), whose dissolved gases show a dominant atmospheric contribution and (ii) hypothermal waters (average temperature of 21 °C), having a meteoritic origin and interacting with both carbonate rocks and inter-bedded evaporitic deposit. Geochemical data allow estimating a geothermal reservoir temperature between 30 °C and 60 °C, according to silica and Ca/Mg geothermometers, respectively. A heat discharge related to hypothermal groundwater flow between 7.75E+06 and 2.00E+07 J/s was computed. δ18O and δ2Η data allowed recognizing a meteoric origin for hypothermal (hereafter TL) waters, with mean recharge (infiltration) elevations between 1300 and 1700 m a.s.l. These waters are gas-rich (e.g., CO2 and He), which amounts are higher than those in air-saturated water (ASW). Carbon and helium isotope signature in the TL waters indicate their mainly crustal origin and involve a tectonic control on fluid migration through the crust. Furthermore, we observe that the He isotopic signature in gases dissolved in TL waters is stable over time and its monitoring could be a powerful tool to assess the seismogenetic processes since their preparatory phases.

New implications for the origin of the IAB main group iron meteorites and the isotopic evolution of the noncarbonaceous (NC) reservoir

The origin of the IAB main group (MG) iron meteorites is explored through consideration of 182W isotopic compositions, thermal modeling of 26Al decay, and mass independent (nucleosynthetic) Mo isotopic compositions of planetesimals formed in the noncarbonaceous (NC) protosolar isotopic reservoir. A refined 182W model age for the meteorites Campo del Cielo, Canyon Diablo, and Nantan suggests that the IAB-MG parent body underwent some form of metal-silicate segregation as early as 5.3 ± 0.4 Myr after calcium-aluminum rich inclusion (CAI) formation or as late as 13.8 ± 1.4 Myr after CAI formation. If melting of the IAB-MG occurred prior to 7 Myr after CAI formation, it was likely driven by 26Al decay for a parent body radius >40 km. Otherwise, additional heat from impact is required for melting metal this late in Solar System history. If melting was partially or wholly the result of internal heating, a thermal model of 26Al decay heat production constrains the accretion age of the IAB-MG parent body to ∼1.7 ± 0.4 Myr after CAI formation. If melting was, instead, dominantly caused by impact heating, thermal modeling suggests the parent body accreted more than 2 Myr after CAI formation. Comparison of Mo mass independent isotopic compositions of the IAB-MG to other NC bodies with constrained accretion ages suggests that the Mo isotopic composition of the NC reservoir changed with time, and that the IAB-MG parent body accreted between 2 to 3 Myr after CAI formation, thus requiring an origin by impact. The relationship between nucleosynthetic Mo isotopic compositions and accretion ages of planetesimals from the NC reservoir suggests that isotopic heterogeneity developed from either addition of s-process material to, or removal of coupled r-/p-process material from the NC reservoir.

Investigation of the Meteorite “Chelyabinsk” by Means of the Positron Annihilation Lifetime and Transmission Mössbauer Spectroscopies

Bulk of the main part of the Chelyabinsk meteorite (ordinary chondrite, LL5) for the presence of nanometer pores therein is investigated by means of the positron annihilation lifetime spectroscopy (PALS). In addition, its phase composition is studied with a help of the transmission Mossbauer spectroscopy (TMS). These results are refined by means of the powder X-ray diffraction (XRD). The obtained data demonstrate an absence of the nanometer pores in the meteorite. TMS data show that the meteorite consists of mineral phases (olivine and pyroxene), which are rather typical for the ordinary chondrites. Iron is present in sulfide and nickel forms. Possible applications of nuclear-physics methods for analysis of an origin of meteorites and evolution of the Solar system are discussed.

Phosphorus-bearing Olivines of Lunar Rocks: Sources and Localization in the Lunar Crust

Abstract—Fragments of P-bearing olivine have been studied in lunar highland, mare, and mingled meteorites and in “Apollo-14”, “Luna-16, -20, -24” lunar samples. The olivines contain up to 0.5 wt % P2O5 and have variable MG# numbers. They are associated with anorthite, pyroxene, and accessory spinel-group minerals, Ti and Zr oxides, phosphates, troilite, and Fe–Ni metal. Three possible sources of P-bearing olivine were found in the lunar material: 1) highland anorthositic–noritic–troctolitic rocks enriched in incompatible elements and interpreted to be related to high-Mg suite rocks: 2) late-stage products of mare basalts crystallization; and 3) unusual olivine–orthopyroxene intergrowths of meteoritic or lunar origin. Enrichment in incompatible elements may result from both crystallization processes (source 2) and KREEP assimilation (sources 1 and 3). However, superimposed metasomatic processes can lead to some addition of phosphorus and other elements. The rarity of P-bearing olivines points either to the low abundance or local distribution of their sources in the lunar crust. Association with mare basalts specifies the highland–mare boundary. The presence of evolved rocks in the studied breccias suggests a possible connection of some sources with recently discovered granitic domes in Procellarum Ocean. This means the P-bearing sources are mainly localized on the nearside of the Moon.

Age and origin of IIE iron meteorites inferred from Hf-W chronology

Abstract Non-magmatic iron meteorites, including the IIE group, can provide important insights into the history of metal-silicate differentiation and collisions on planetesimals. To better constrain the evolution of metal segregation and impacts on the IIE parent body, W isotopic data are reported for 10 IIE iron meteorites and a metal vein from the Portales Valley H6 chondrite. In addition, Pt isotopic data were obtained to quantify cosmic ray-induced neutron capture effects on W isotopes. After correction for these effects, the IIE iron meteorites exhibit variable pre-exposure 182W compositions, translating into Hf-W model age clusters of ∼4–5 million years (Ma), ∼10 Ma, ∼15 Ma, and ∼27 Ma after CAI formation. These distinct 182W clusters likely represent samples from several discrete metallic melt pools on the IIE parent asteroid. The earliest metal segregation event at ∼4–5 Ma was likely facilitated by 26Al decay as an internal heat source. By contrast, the younger Hf-W model ages may not be chronologically meaningful, and probably reflect the effects of secondary mixing and re-equilibration of metal and silicates, likely facilitated by impacts on the IIE parent body. Thus, contrary to prior work, the Hf-W systematics of IIE iron meteorites do not require a protracted history of metal-silicate separation on the IIE parent body. Instead the results of this study are fully consistent with a single partial metal-silicate differentiation event driven by endogenic heating at ∼4–5 Ma, followed by one or multiple impact events causing mixing and re-equilibration of metal and silicates at a later stage. The exact timing of these impact event(s) remains poorly constrained, but they most likely occurred in the first few tens of Ma of Solar System history.

Meteoritic iron artefacts redux

The earliest iron artefacts are often presented as products made of meteoritic iron, which is characterised by its high iron content. However, recent studies have shown that high nickel and iron content cannot be taken as a firm criterion for establishing its meteoritic origin. The most effective tool for helping to specify the elemental composition in such cases is a metallographic analysis. It turns out that the material of many artefacts regarded as having been forged from meteoritic iron could in fact be bloomery iron. An analysis of ample yet scattered evidence suggests that the production of items from meteoritic iron could in fact be irregular and sporadic.

In search of historical roots of the meteorite impact theory: Franz von Paula Gruithuisen as the first proponent of an impact cratering model for the Moon in the 1820s

AbstractFranz von Paula Gruithuisen (1774–1852), the Bavarian medic, physician, and astronomer, enfant terrible of German science, is known for his insightful observations and many extravagant conceptions. However, since the seminal monograph of Baldwin (1949), he is also referenced for early contributions to the meteoritic origin concept of lunar craters. His most commonly cited paper of 1828 is analyzed here for the first time in some detail. For Gruithuisen, impact phenomena were only an outcome of a more general cosmogenic theory, which assumed planet and satellite growth by concentric shell‐like coalescence of the cosmic bodies. The aggregation theory thus defined was initiated in 1794 by Chladni, developed by the Bierberstein brothers and Anton Zach. Gruithuisen was notably the first person to formulate a nascent concept of lunar crater mechanics. This cratering process, as he thought, is based on an uneven gravitational subsidence of concentrically layered spherical impactors (=the solid core of comet) into the plastic sediments. Only the more resistant and heavy central portion of the body was submerging deeper, and therefore, the circular terrace‐like rim of the ring mountains was formed. Gruithuisen tried also to recognize terrestrial equivalents of large‐scale crater‐like mountains on the Moon, and speculated on other impact consequences, such as a catastrophic influence on the history of the biosphere and a cometary source of the terrestrial hydrosphere. These ideas found several conceptual followers in the vital German science of the last decades of 19th century. Thus, despite principal errors in the gravitationally penetrative cratering model, we confirm the claim of recognition of Gruithuisen as one of the founders of the impact hypothesis.

Challenges of identifying putative planetary-origin meteorites of non-igneous material

This paper summarizes the challenges of identifying planetary-origin meteorites of non-igneous composition - particularly those of sedimentary origin. Evidence for putative sedimentary-origin (sed-type) meteorites and their potential parent bodies is reviewed, suggesting that the list of candidate parent bodies for sed-type meteorites includes, but is not limited to, Mars, Enceladus, Ganymede, Europa, Ceres, Vesta, and other hypothetical planets that existed between the orbits of Mars and Jupiter in the past. The extraterrestrial origin and probable parent body for sed-type meteorites should be assessed based on multiple lines of evidence, and not solely limited to tests of oxygen and noble gas isotopes, whose signatures may undergo terrestrial contamination and which may exhibit significant heterogeneity within both the Solar System and parent cosmic bodies. The observed fall of a cosmic body, evidence of hypervelocity fall, signs of impact, presence of fusion crust, melting, and/or shock deformation features in impactor fragments should be considered as priority signs of meteoritic origin.

Investigating the subsurface structure of the main crater of the proposed Sirente meteorite crater field (Central Italy): new clues from reflection seismics

The Sirente crater field (Central Italy) consists of a main, ≈130 m wide, droplet-shaped in plan view depression with a prominently elevated rim, and 30 smaller depressions in its close vicinity. It was discovered in 2002 and proposed to be of meteorite impact origin based on its geological and geomorphological similarities to known crater fields. It is developed in non-lithified lake sediments (i.e. carbonate mud). Given the age of formation in the 3rd to 5th centuries A.D., the inferred catastrophic origin was, in the media, soon related to the celestial sign (“Chi Rho”) said to have been seen by Emperor Constantine in 312 A.D. and suggested to have changed the course of both Roman and Christian history. However, the meteoritic origin is not yet confirmed and has been contested. This work presents new geophysical data on the subsurface structure of the main crater, which provides further clues around the controversy of its origin. Two roughly transversal seismic reflection profiles across the main crater reveal a deep (53 m on average), rootless, bowl-shaped structure with a poorly developed, deep-seated central mound, as well as different seismic facies representing a crater infill of disturbed material resembling the breccia lens in craters formed in rock. This survey also allowed the recognition of possible compaction-fissures and upturned strata below the rim, similar to what is known from explosion craters in porous, unconsolidated targets. Some of these structures had already been noted in published resistivity surveys (ERT). The structural features noted in this geophysical survey are consistent with the impact hypothesis and do not support other proposed mechanisms of formation such as karst or mud volcano.

Corrigendum to “Meteoritic origin and manufacturing process of iron blades in two Bronze Age bimetallic objects from China” [J. Cult. Herit. 30 (2018) 45–50

Corrigendum to “Meteoritic origin and manufacturing process of iron blades in two Bronze Age bimetallic objects from China” [J. Cult. Herit. 30 (2018) 45–50

Alpha Centauri System and Meteorites Origin

We propose a mathematical model for determining the probability of meteorite origin, impacting the earth. Our method is based on axioms similar to both the complex networks and emergent gravity. As a consequence, we are able to derive a link between complex networks and Newton’s gravity law, and as a possible application of our model we discuss several aspects of the Bacubirito meteorite. In particular, we analyze the possibility that the origin of this meteorite may be alpha Centauri system. Moreover, we find that in order for the Bacubirito meteorite to come from alpha Cen and be injected into our Solar System, its velocity must be reduced one order of magnitude of its ejected scape velocity from alpha Cen. There are several ways how this could happened, for example through collision with the Oort cloud objects (located outside the boundary of our Solar System), and/or through collisions within the Solar meteorites belt (located between Mars and Jupiter). We also argue that it may be interesting to study the Bacubirito meteorite from the perspective of the recently discovered Oumuamua object.

Meteoritic origin and manufacturing process of iron blades in two Bronze Age bimetallic objects from China

Abstract It is widely accepted that meteoritic iron was the first iron alloy used by mankind, however, the manufacturing processes of the earliest iron artefacts remain uncertain and sometimes disputed. Here, we present both chemical and microanalytical results of samples from two bimetallic objects from Bronze Age central China. It is confirmed that the blades were made of meteoritic iron. In-situ photomicrograph and detailed microanalysis provides solid evidence for the cast-on and hot-work processes. We also demonstrate that significant information can be extracted through multiple analyses despite the severely corroded condition of ancient iron objects.

Numerical modeling of the 2013 meteorite entry in Lake Chebarkul, Russia

Abstract. The results of the numerical simulation of possible hydrodynamic perturbations in Lake Chebarkul (Russia) as a consequence of the meteorite fall of 2013 (15 February) are presented. The numerical modeling is based on the Navier–Stokes equations for a two-phase fluid. The results of the simulation of a meteorite entering the water at an angle of 20° are given. Numerical experiments are carried out both when the lake is covered with ice and when it is not. The estimation of size of the destructed ice cover is made. It is shown that the size of the observed ice hole at the place of the meteorite fall is in good agreement with the theoretical predictions, as well as with other estimates. The heights of tsunami waves generated by a small meteorite entering the lake are small enough (a few centimeters) according to the estimations. However, the danger of a tsunami of meteorite or asteroid origin should not be underestimated.

Possible Fengyun-1C debris fall

A fall of small objects took place on 27th April 2012 in Wargowo village near Oborniki, about 25km NW from Poznań (Poland). There was only one eye-witness of the fall, who found two separate pieces (ca. 2.7cm and ca. 2cm), with several small additional fragments. After microscopic observations and chemical analysis a meteoritic origin of these objects was excluded. They are identified as space debris, therefore man-made. The most probable source of the observed fall was space debris 35127 Fengyun 1C DEB, created during destruction of the Chinese weather satellite Fengyun-1C (FY-1C).

Είμαστε μόνοι στο συμπάν; Οι μετεωρίτες δίνουν απαντήσεις;

The humankind, despite the recent technological achievements, does not yet have the ability to carry out routine trips to nearby celestial bodies. However, space science is a reality. The “Apollo” missions, that took place during the period 1969-1972, included the moon landing, the walk of astronauts and collection of valuable samples. Since then, no similar space journey has been carried out. The possibility for future missions such as the return to the Moon or Mars, or to an asteroid (e.g., Vesta), seems small enough to be implemented in the next decades. Nevertheless, nature has the mechanism and procedures to resolve this problem by sending extra-terrestrial rocks in earth in the form of meteorites. Meteorite fall on Earth is a major event, as it reveals important information about the primordial stages of formation of our solar system, or the creation processes of other planets. However, the big question still remains; whether these rocks host or have traces of past life in turn employs researchers in the last twenty years. McKay et al. (1996) studied the meteorite ALH 84001 originating from Mars, claimed for important discoveries such as structures corresponding to nanobacteria. In the current paper, we focus on the origin of Martian meteorites, presenting their complete geological history; from the genesis of their protoliths till their falling to the earth. We attempt to shade light in the understanding of meteorite formation using mineralogical-petrological-geochemical data, and the assignment of timing for each event based upon contemporary geochronological data. Recently, studies of the Martian meteorite Tissint, allegedly discovered structures rich in carbon and oxygen. Furthermore, recent field observations from Curiosity rover, indicates the existence of surface water that flowed once in the past at the Martian surface. We conclude that the planet Mars might not be a "dead" planet. But it turns out that many of the meteorites that reach the Earth, have undergone a complex history which is associated with the development of very high pressures and temperatures on the surface of the planet (e.g., Mars) from which they originate, able to destroy any trace of life before them. After all, we should be very sceptic and evaluate all the possibilities before the acceptance for the existence of life out there.

Characterization and 10Be content of iron carbonate concretions for genetic aspects – Weathering, desert varnish or burning: Rim effects in iron carbonate concretions

The research investigated three iron carbonate (siderite) sedimentary concretions from Nagykovácsi, Úri and Délegyháza, Hungary. To identify possible source rocks and effects of the glaze-like exposed surface of the concretions, we carried on comparative petrological, mineralogical, geochemical and isotopic studies. The samples were microbially mediated siderite concretions with embedded metamorphous and igneous mineral clasts, and had specific rim belts characterized by semi-concentric outer Fe-oxide layers, fluffy pyrite-rich outer belts and siderite inner parts. We investigated the cross section of the Fe-carbonate concretions by independent methodologies in order to identify their rim effects. Their surficial oxide layers showed evidence of degassing of the exposed surface caused most probably by elevated temperatures. The inner rim pyrite belt in the concretions excluded the possibility of a prolonged wet surface environment. Microtextural and mineralogical features did not support desert varnish formation. 10Be nuclide values of the Nagykovácsi and Uri concretions were far above the level of terrestrial in-situ cosmogenic nuclides, but they were consistent with the lowest levels for meteorites. Though the data were not conclusive to confirm any kind of known origin, they are contradictary, and open possibilities for a scenario of terrestrial meteorite origin.

The meteoritic origin of Tutankhamun's iron dagger blade

AbstractScholars have long discussed the introduction and spread of iron metallurgy in different civilizations. The sporadic use of iron has been reported in the Eastern Mediterranean area from the late Neolithic period to the Bronze Age. Despite the rare existence of smelted iron, it is generally assumed that early iron objects were produced from meteoritic iron. Nevertheless, the methods of working the metal, its use, and diffusion are contentious issues compromised by lack of detailed analysis. Since its discovery in 1925, the meteoritic origin of the iron dagger blade from the sarcophagus of the ancient Egyptian King Tutankhamun (14th C. BCE) has been the subject of debate and previous analyses yielded controversial results. We show that the composition of the blade (Fe plus 10.8 wt% Ni and 0.58 wt% Co), accurately determined through portable x‐ray fluorescence spectrometry, strongly supports its meteoritic origin. In agreement with recent results of metallographic analysis of ancient iron artifacts from Gerzeh, our study confirms that ancient Egyptians attributed great value to meteoritic iron for the production of precious objects. Moreover, the high manufacturing quality of Tutankhamun's dagger blade, in comparison with other simple‐shaped meteoritic iron artifacts, suggests a significant mastery of ironworking in Tutankhamun's time.

Heinrich Wänke (1928–2015)

Heinrich Wänke (1928–2015)