Dark Lithology Research Articles

Chondrules from the ordinary chondrite Itawa Bhopji (L3-5): Noble gases and nitrogen

Noble gases and nitrogen compositions are investigated in chondrules of Itawa Bhopji (L3-5) chondrite. Single chondrule and bunch of chondrules were analysed in this work. Isotopic ratios of noble gases in chondrules indicate mixture of Q-HL-SW and cosmogenic. The cosmic ray exposure age of the chondrules using 21Ne are 30.0 ± 2.3 and 25.9 ± 2.5 Ma. No excess cosmic ray exposure (CRE) age observed in the chondrules from that of bulk aliquot of dark lithology. The trapped nitrogen signature, δ15Nt in the chondrules, is +15.8 ± 2.2‰ (bunch of chondrules) and +15.1 ± 2.3‰ (single chondrule). Trapped nitrogen isotopic signature in chondrules differs from dark and light lithology of the meteorite and it is also distinct from metal separates. Trapped nitrogen composition in chondrules differs than Q-phase, solar wind (SW) and HL components. This implies that chondrules in Itawa Bhopji (L3-5) chondrite composed of isotopically distinct component than any of the known reservoir. Distinct trapped nitrogen isotopic signatures in the constituents of a meteorite indicates their formation at various places with the heliocentric distance. The abundance of nitrogen in chondrules is 6.14 ± 0.51 ppm (bunch) and 5.71 ± 0.48 ppm (single). Radiogenic 129Xe from the decay of 129I was observed in chondrules, indicative of their formation in early solar system.

Physical Characterization of Near-Earth Asteroid (52768) 1998 OR2: Evidence of Shock Darkening/Impact Melt

We conducted photometric and spectroscopic characterization of near-Earth asteroid (52768) 1998 OR2 during a close approach to Earth in 2020 April. Our photometric measurements confirm the rotation period of the asteroid to be 4.126 ± 0.179 hr, consistent with the previously published value of 4.112 ± 0.001 hr. By combining our visible spectroscopic measurements (0.45–0.93 μm) with archival MITHNEOS near-infrared spectra (0.78–2.49 μm), we classify the asteroid as an Xn-type in the Bus–DeMeo taxonomy. The combined spectrum shows two weak absorption bands: Band I at 0.926 ± 0.003 μm and Band II at 2.07 ± 0.02 μm, with band depths of 4.5% ± 0.15% and 4.0% ± 0.21%, respectively. The band area ratio is 1.13 ± 0.05. These spectral band parameters plot at the tip of the S(IV) region of the Gaffey S-asteroid subtypes plot, suggesting an affinity to ordinary chondrite meteorites. We calculated the chemistry of olivine and pyroxene using the Band I center to be 20.1 ± 2.3 mol% fayalite and 18.2 ± 1.5 mol% ferrosilite, consistent with H-chondrites. Principal component analysis of 1998 OR2's combined visible–near-IR spectrum falls on the C/X-complex side of the α-line, near the end of the shock-darkening trend, consistent with its weak absorption bands (band depth <5%). We use an areal mixing model with lab measurements of the shock-darkened H5 chondrite, Chergach, to constrain the amount of shock-darkened material on the asteroid’s surface at ∼63% dark lithology and ∼37% light lithology.

Microtextures in the Chelyabinsk impact breccia reveal the history of Phosphorus‐Olivine‐Assemblages in chondrites

AbstractThe geochemistry and textures of phosphate minerals can provide insights into the geological histories of parental asteroids, but the processes governing their formation and deformation remain poorly constrained. We assessed phosphorus‐bearing minerals in the three lithologies (light, dark, and melt) of the Chelyabinsk (LL5) ordinary chondrite using scanning electron microscope, electron microprobe, cathodoluminescence, and electron backscatter diffraction techniques. The majority of studied phosphate grains appear intergrown with olivine. However, microtextures of phosphates (apatite [Ca5(PO4)3(OH,Cl,F)] and merrillite [Ca9NaMg(PO4)7]) are extremely variable within and between the differently shocked lithologies investigated. We observe continuously strained as well as recrystallized strain‐free merrillite populations. Grains with strain‐free subdomains are present only in the more intensely shocked dark lithology, indicating that phosphate growth predates the development of primary shock‐metamorphic features. Complete melting of portions of the meteorite is recorded by the shock‐melt lithology, which contains a population of phosphorus‐rich olivine grains. The response of phosphorus‐bearing minerals to shock is therefore hugely variable throughout this monomict impact breccia. We propose a paragenetic history for P‐bearing phases in Chelyabinsk involving initial phosphate growth via P‐rich olivine replacement, followed by phosphate deformation during an early impact event. This event was also responsible for the local development of shock melt that lacks phosphate grains and instead contains P‐enriched olivine. We generalize our findings to propose a new classification scheme for Phosphorus‐Olivine‐Assemblages (Type I–III POAs). We highlight how POAs can be used to trace radiogenic metamorphism and shock metamorphic events that together span the entire geological history of chondritic asteroids.

Post-impact metamorphism of the Chelyabinsk meteorite in shock experiment

The vast majority of the studied samples of the Chelyabinsk LL5 meteorite shower is represented by the light, dark and impact melt lithologies. Their regular relative positions were revealed in the sections of the large fragments of the Chelyabinsk meteorite. Thus, the zones of light lithology are surrounded by the zones of dark lithology and they both are located within the impact melt. In the present study, we compare the breccia texture of large samples with the lithology zones formed after shock experiment. It was shown that during the spherical shock experiment performed using the light lithology material of the Chelyabinsk meteorite, the gradient of P-T conditions was realized so that dark lithology, mixed lithology, and impact melt were formed within one shock experiment. In the present study, we focus on structural changes associated with metal and troilite. The formation mechanism of the breccia texture in the large fragments of the Chelyabinsk meteoroid was proposed.

Variability of Chelyabinsk meteoroid stones studied by Mössbauer spectroscopy and X-ray diffraction.

The meter-scale variations of material properties of the 20-m sized Chelyabinsk meteoroid are critical for understanding why the meteoroid fragmented the way it did and caused the devastating airburst that sent over 1600 people to the hospital for treatment of glass cuts and minor injuries on February 15, 2013. From a range of differently looking unweathered meteorite fragments that were recovered shortly after the event, these material differences were probed by means of optical and scanning electron microscopy, X-ray diffraction (XRD), and the high velocity resolution Mössbauer spectroscopy. All main and some minor iron-bearing phases were identified on the basis of XRD data and Mössbauer spectra. The Fe2+ partitioning between the M1 and M2 sites in silicate phases was determined independently using XRD and Mössbauer data. Different meteorite fragments show a range of 570-1180 K in the temperature of the Fe2+ and Mg2+ equilibrium distribution between the M1 and M2 sites in olivine, while that in orthopyroxene falls in the range 870-1180 K (these ranges were estimated using both techniques). This fact points out a slightly different thermal history of these minerals before they accumulated in different parts of the Chelyabinsk meteoroid. The Chelyabinsk meteoroid is a fragmental breccia from materials formed at different depths in their parent body, or from materials that experienced different annealing temperatures in impacts. In addition, the fusion crust from two fragments, studied by XRD and Mössbauer spectroscopy, experienced a different thermal history during entry, suggesting that the fragment with mixed light and dark lithologies was located deeper inside the initial meteoroid than the fragment with only light lithology, or fragmented less readily.

The Chelyabinsk meteorite: New insights from a comprehensive electron microscopy and Raman spectroscopy study with evidence for graphite in olivine of ordinary chondrites

AbstractWe present results of petrographic, mineralogical, and chemical investigations of three Chelyabinsk meteorite fragments. Three distinct lithologies were identified: light S3 LL5, dark S4–S5 LL5 material, and opaque fine‐grained former impact melt. Olivine–spinel thermometry revealed an equilibration temperature of 703 ± 23 °C for the light lithology. All plagioclase seems to be secondary, showing neither shock‐induced fractures nor sulfide‐metal veinlets. Feldspathic glass can be observed showing features of extensive melting and, in the dark lithology, as maskelynite, lacking melt features and retaining grain boundaries of former plagioclase. Olivine of the dark lithology shows planar deformation features. Impact melt is dominated by Mg‐rich olivine and resembles whole‐rock melt. Melt veins (&lt;2 mm) are connected to narrower veinlets. Melt vein textures are similar to pegmatite textures showing chilled margins, a zone of inward‐grown elongated crystals and central vugs, suggesting crystallization from supercooled melt. Sulfide‐metal droplets indicate liquid immiscibility of both silicate and sulfide as well as sulfide and metal melts. Impact melting may have been an important factor for differentiation of primitive planetary bodies. Graphite associated with micrometer‐sized melt inclusions in primary olivine was detected by Raman mapping. Carbon isotopic studies of graphite could be applied to test a possible presolar origin.

IDENTIFIKASI VISUAL BATUAN PAF DAN NAF STUDI KASUS DI PT ARUTMIN INDONESIA ASAM ASAM

The research location is in Asam-Asam PT Arutmin Indonesia, located in District Jorong, Tanah Laut, Kalimantan Selatan. This study aims to determine the relationship of visual rock with PAF and NAF rock properties based on the distribution pattern, volume, and utilization. Visual identification that shows the strong correlation of PAF on the grain size of silt, color dark gray lithology, and lithologic silt. a strong correlation was also found on NAF rock with a grain size of clay, fine sand, very fine sand. In the color white rock medium, medium gray, light gray. obtained a volume of PAF: 208 309 329 BCM, NAF = 200 764 182 BCM volume, so the volume of NAF to be taken can coat 3,5 meters disposal.

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X‐ray map of a thin section of a sample of the Chelyabinsk meteorite from the study of Righter et al. (pp. 1790–1819). Sample Chel‐102 contains roughly 50 modal% of a dark lithology that is shock‐darkened LL5 chondrite (left side of image). There is heavy veining of this portion, and very little original equilibrated chondritic texture remaining. The other 50% of Chel‐102 (right side of image) is a very fi ne‐grained melt breccia comprised of mesostasis (85%), metal‐troilite droplets (5%), and chondritic fragments of similar mineralogy to the light lithology of Chel‐101. Image produced by Eve. L. Berger.

Mineralogy, petrology, chronology, and exposure history of the Chelyabinsk meteorite and parent body

AbstractThree masses of the Chelyabinsk meteorite have been studied with a wide range of analytical techniques to understand the mineralogical variation and thermal history of the Chelyabinsk parent body. The samples exhibit little to no postentry oxidation via Mössbauer and Raman spectroscopy indicating their fresh character, but despite the rapid collection and care of handling some low levels of terrestrial contamination did nonetheless result. Detailed studies show three distinct lithologies, indicative of a genomict breccia. A light‐colored lithology is LL5 material that has experienced thermal metamorphism and subsequent shock at levels near S4. The second lithology is a shock‐darkened LL5 material in which the darkening is caused by melt and metal‐troilite veins along grain boundaries. The third lithology is an impact melt breccia that formed at high temperatures (~1600 °C), and it experienced rapid cooling and degassing of S2 gas. Portions of light and dark lithologies from Chel‐101, and the impact melt breccias (Chel‐102 and Chel‐103) were prepared and analyzed for Rb‐Sr, Sm‐Nd, and Ar‐Ar dating. When combined with results from other studies and chronometers, at least eight impact events (e.g., ~4.53 Ga, ~4.45 Ga, ~3.73 Ga, ~2.81 Ga, ~1.46 Ga, ~852 Ma, ~312 Ma, and ~27 Ma) are clearly identified for Chelyabinsk, indicating a complex history of impacts and heating events. Finally, noble gases yield young cosmic ray exposure ages, near 1 Ma. These young ages, together with the absence of measurable cosmogenic derived Sm and Cr, indicate that Chelyabinsk may have been derived from a recent breakup event on an NEO of LL chondrite composition.

Chelyabinsk meteorite: Shock metamorphism, black veins and impact melt dikes, and the Hugoniot

The Chelyabinsk meteorite (which fell on February 15, 2013) is a LL5 chondrite of shock stage S4, whose fragments are classified into light and dark lithologies. According to the intensity of their shock metamorphism, light lithology fragments are subdivided into two groups, which were affected by peak pressures within the ranges of 20–25 and 25–30 GPa, respectively. The material of the dark lithology was shocked at 25–30 GPa but was then annealed, which resulted in a decrease in the discernible degree of shock metamorphism. Black veins cutting across both the light and the dark lithologies and impact melt dikes in the dark lithology were produced by friction melting along boundaries of blocks that had been generated by fragmentation in a shock wave. The impact melt of the dikes is slightly enriched in Si, Al, Ca, Na, and K and has an oxygen isotopic composition similar to the chondrite matrix. It is thought that black vein melt started to crystallize in a rarefaction wave. Melt in the dikes and the central portions of the black veins crystallized after total pressure release. Heating of material hosting the melt dikes resulted in its blackening and annealing of its shock metamorphic features. The Hugoniot obtained for the Chelyabinsk meteorite was utilized to calculate the post-shock and shock temperatures within a broad pressure range. According to these evaluations, the meteorite was heated for 65–135 degrees during the impact event. The melting of the LL chondrite started at a load of approximately 100 GPa because of the high “equilibrium” post-shock temperatures, and a pressure of 140 GPa resulted in the complete melting of the material.

Magnetic properties of the LL5 ordinary chondrite Chelyabinsk (fall of February 15, 2013)

AbstractHere we characterize the magnetic properties of the Chelyabinsk chondrite (LL5, S4, W0) and constrain the composition, concentration, grain size distribution, and mineral fabric of the meteorite's magnetic mineral assemblage. Data were collected from 10 to 1073 K and include measurements of low‐field magnetic susceptibility (χ0), the anisotropy of χ0, hysteresis loops, first‐order reversal curves, Mössbauer spectroscopy, and X‐ray microtomography. The REM and REM′ paleointensity protocols suggest that the only magnetizations recorded by the chondrite are components of the Earth's magnetic field acquired during entry into our planet's atmosphere. The Chelyabinsk chondrite consists of light and dark lithologies. Fragments of the light lithology show logχ0 = 4.57 ± 0.09 (s.d.) (n = 135), while the dark lithology shows 4.65 ± 0.09 (n = 39) (where χ0 is in 10−9 m3 kg−1). Thus, Chelyabinsk is three times more magnetic than the average LL5 fall, but is similar to a subgroup of metal‐rich LL5 chondrites (Paragould, Aldsworth, Bawku, Richmond) and L/LL5 chondrites (Glanerbrug, Knyahinya). The meteorite's room‐temperature magnetization is dominated by multidomain FeNi alloys taenite and kamacite (no tetrataenite is present). However, below approximately 75 K remanence is dominated by chromite. The metal contents of the light and dark lithologies are 3.7 and 4.1 wt%, respectively, and are based on values of saturation magnetization.

Magnetic properties of the Chelyabinsk meteorite: Preliminary results

This paper presents the distribution of magnetic susceptibility, χ0, in fragments of the Chelyabinsk ordinary chondrite (LL5, S4, W0, fall of February 15, 2013) from the collection of the Vernadsky Institute of Geochemistry and Analytical Chemistry, Russian Academy of Sciences, and results obtained by standard magnetic techniques for the meteorite material, including thermomagnetic analysis, measurements of natural remanent magnetization (NRM) and saturation isothermal remanent magnetization (SIRM), as well as the spectra of their alternating field demagnetization at amplitudes up to 170 mT, measurements of hysteresis loops and back-field remanence demagnetization curves at temperatures from 10 K to 700°C etc. The mean logχ0 values for the light-colored (main) lithology of the meteorite material and impact-melt breccia from our collection are 4.54 ± 0.10 (n = 66) and 4.65 ± 0.09 (n = 38) (×10−9 m3/kg), respectively. According to international magnetic classification of meteorites, Chelyabinsk falls within the range of LL5 chondrites. The mean metal content was estimated from the saturation magnetization, Ms, of the light- and dark-colored lithologies as 3.7 and 4.1 wt %, respectively. Hence, the dark lithology is richer in metal. The metal grains are multidomain at room temperature and show low coercive force, Bc ( 75 K. In the temperature range below 75 K, magnetic properties are controlled by chromite; the magnetic hardness of the samples is maximal at 10 K and equals to 606 and 157 mT for the light- and dark-colored lithologies, respectively.

The fall, recovery, and classification of the Park Forest meteorite

Abstract— On the night of March 26, 2003, a large meteorite broke up and fell upon the south suburbs of Chicago. The name Park Forest, for the village that is at the center of the strewnfield, has been approved by the nomenclature committee of the Meteoritical Society. Satellite data indicate that the bolide traveled from the southwest toward the northeast. The strewnfield has a southeast‐northwest trend; however, this is probably due to the effects of strong westerly winds at high altitudes. Its very low 56Co and very high 60Co activities indicate that Park Forest had a preatmospheric mass that was at least ∼900 kg and could have been as large as ∼7 times 103 kg, of which only ∼30 kg have been recovered. The average compositions of olivine and low‐Ca pyroxene, Fa24.7 ± 1.1 and Fs20.8 ± 0.7, respectively, and its bulk oxygen isotopic composition, δ18O = +4.68%o, δ17O = +3.44%o, show that Park Forest is an L chondrite. The ferromagnesian minerals are well equilibrated, chondrules are easily recognized, and maskelynite is mostly ≤50 μm across. Based on these observations, we classify Park Forest as type 5. The meteorite has been strongly shocked, and based on the presence of maskelynite, mosaicism and planar deformation features in olivine, undulatory extinction in pyroxene, and glassy veins, the shock stage is S5. The meteorite is a monomict breccia, consisting of light‐colored, angular to rounded clasts in a very dark host. The light and dark lithologies have essentially identical mineral and oxygen isotopic compositions. Their striking difference in appearance is due to the presence of a fine, pervasive network of sulfide veins in the dark lithology, resulting in very short optical path lengths. The dark lithology probably formed from the light lithology in an impact that formed a sulfide‐rich melt and injected it into cracks.

Solar wind and other gases in the regoliths of the Pesyanoe parent object and the moon

We report new data from Pesyanoe‐90,1 (dark lithology) on the isotopic signature of solar wind (SW) Xe as recorded in this enstatite achondrite which represents a soil‐breccia of an asteroidal regolith. The low temperature (≤800°C) steps define the Pesyanoe‐S xenon component, which is isotopically consistent with SW Xe reported for the lunar regolith. This implies that the SW Xe isotopic signature was the same at two distinct solar system locations and, importantly, also at different times of solar irradiation. Further, we compare the calculated average solar wind “SW‐Xe” signature to Chass‐S Xe, the indigenous Xe observed in SNC (Mars) meteorites. Again, a close agreement between these compositions is observed, which implies that a mass‐dependent differential fractionation of Xe between SW‐Xe and Chass‐S Xe is &gt;1.5%o per amu. We also observe fractionated (Pesyanoe‐F) Xe and Ar components in higher temperature steps and we document a fission component due to extinct 244Pu. Interestingly, the Pesyanoe‐F Xe component is revealed only at the highest temperatures (&gt;1200°C). The Pesyanoe‐F gas reveals Xe isotopic signatures that are consistent with lunar solar energetic particles (SEP) data and may indicate a distinct solar energetic particle radiation as was inferred for the moon. However, we cannot rule out fractionation processes due to parent body processes. We note that ratios 36Ar/38Ar≤5 are also consistent with SEP data. Calculated abundances of the fission component correlate well with radiogenic 40Ar concentrations, revealing rather constant 244Pu/K ratios in Pesyanoe, and separates thereof, and indicate that both components were retained. We identify a nitrogen component (δ15N = 44%o) of non‐solar origin with an isotopic signature distinct from indigenous N (δ15N = −33%o). While large excesses at 128Xe and 129Xe are observed in the lunar regolith samples, these excesses in Pesyanoe are small. On the other hand, significant 126Xe isotopic excesses, comparable to relative excesses observed in lunar soils and breccias, are prominent in the intermediate temperature steps of Pesyanoe‐90,1.

Itawa Bhopji (L3–5) chondrite regolith breccia: Fall, classification, and cosmogenic records

Abstract— A stony meteorite fell at Itawa Bhopji, Rajasthan, India on 2000 May 30. This is the fifth recorded fall in a small area of Rajasthan during the past decade. The meteorite is an ordinary chondrite with light clasts in a dark matrix, consisting of a mixture of equilibrated (mainly type 5) and unequilibrated components. Olivine is Fa24–26 and pyroxene Fs20–22 but, within the unequilibrated components, olivine (Fa5–29) and low calcium pyroxene (Fs5–37) are highly variable. Based on petrographic studies and chemical analyses, it is classified as L(3–5) regolith breccia. Studies of various cosmogenic records, including several gamma‐emitting radionuclides varying in half‐life from 5.6 day 52Mn to 0.73 Ma 26Al, tracks and rare gases have been carried out. The exposure age of the meteorite is estimated from cosmogenic components of rare gases to be 19.6 Ma. The track density varies by a factor of ˜3 (from 4 to 12 times 106/cm2) within the meteorite, indicating a preatmospheric body of ˜9 cm radius (corresponding to a meteoroid mass of ˜11 kg) and small ablation (1.5 to 3.6 cm). Trapped components in various rare gases are high and the solar component is present in the dark portion of the meteorite. Large excess of neutron‐produced 82Kr and 128Xe in both the light and the dark lithology but very low 60Co, indicating low neutron fluxes received by the meteoroid in the interplanetary space, are clear signatures of an additional irradiation on the parent body.

Magombedze: A new H‐chondrite with light‐dark structure

Abstract— Magombedze is a light‐dark structured H‐chondrite breccia that fell in Zimbabwe on 1990 July 2 at 15:30 GMT. White clasts are moderately shocked and have equilibrated mafic silicates (pyroxene Fs16–18, olivine Fa18–19) together with clear optically‐recognizable plagioclase of variable composition (An9–13 found); chondrules are distinct but contain no trace of preserved glass. The darker surrounding material contains a higher proportion of fine‐grained metal and sulfide than the white clasts, and many of its constituent grains show little evidence of shock. Mafic silicates in the dark lithology are distinctly less‐equilibrated (pyroxene Fs5–21, olivine Fa11–20) than those in the white clasts, and many chondrules preserve brown devitrified glass; some metamorphic plagioclase of variable composition (An11–22, found) is present. Some monoclinic pyroxene occurs in both fractions, but it is relatively common in the dark fraction. The white clasts are classified as H5, and the enclosing dark material is H3–5.

The Shaw meteorite: History of a chondrite consisting of impact-melted and metamorphic lithologies

The Shaw L-group chondrite consists of three intermingled lithologies. One is light-colored and has a poikilitic texture, consisting of olivine (many skeletal and euhedral) and augite crystals surrounded by larger (up to 1 mm) orthopyroxene grains; plagioclase occurs between orthopyroxene crystals and rare, small (<5 μm) patches of Si-K-rich glass or cryptocrystalline material occurs within the plagioclase. The skeletal olivine crystals contain 0.08–0.16 wt% CaO. Petrofabric measurements show that the c-axes of the olivines are aligned. The light-colored lithology also contains numerous vugs and vesicles: SEM studies reveal euhedral, possibly vapor-deposited, crystals of olivine and pyroxene in the vugs. A second lithologic type is dark-colored, contains remnant chondrules. and has a microgranular texture. Poikilitic orthopyroxene crystals, where present, are smaller (0.1–0.2mm) than they are in the light-colored lithology. Microgranular olivine crystals contain <0.08 wt% CaO: most contain 0.03–0.05 wt% CaO. Vugs are rare and Si-K-rich material is absent. The third lithologic type is gray macroscopically and seems to be intermediate between the other two. It has a well-developed poikilitic texture, but contains neither skeletal olivines (euhedral olivines are rare) nor Si-K-rich material: remnant chondrules are present but less abundant than in the dark lithology. A modal analysis of a 5300 mm 2 slab shows, contrary to published opinions, that Shaw contains normal L-group chondrite abundances of metal and troilite. However, these phases are distributed irregularly throughout the meteorite. The light colored lithology is nearly devoid of metal and troilite and centimeter-sized metal-troilite globules occur between the three silicate lithologies. Wherever the metal occurs, it consists of nearly homogeneous martensite (13.9 wt% Ni) rimmed by kamacite (7.1 wt% Ni). These data indicate that Shaw is a partly-melted shock-breccia. The light-colored lithology must have been totally melted, as shown by the presence of aligned. CaO-rich, skeletal olivines; Si-K-rich residual material: and vugs and vesicles lined with euhedral crystals of mafic silicates. The dark areas appear to be unmelted target rock of L-group composition. Analysis of the growth of kamacite at the taenite (now martensite) borders indicates a cooling rate of ~ 3 C/10 3 yr. or one thousand times faster than most ordinary chondntes. The Shaw impact event probably formed a crater several kilometers in diameter on its meteorite parent body.