Meteorite Shower Research Articles

The Santa Filomena meteorite shower: Trajectory, classification, and opaque phases as indicators of metamorphic conditions

AbstractOn August 19, 2020, at 13:18—UTC, a meteor event ended as a meteorite shower in Santa Filomena, a city in the Pernambuco State, northeast Brazil. The heliocentric orbital parameters resulting from images by cameras of the weather broadcasting system were semimajor axis a = 2.1 ± 0.1 au, eccentricity e = 0.55 ± 0.03, and inclination i = 0.15o ± 0.05. The data identified the body as an Apollo object, an Earth‐crossing object with a pericenter interior to the Earth's orbit. The chemical, mineralogical, and petrological evaluations, as well as the physical analysis, followed several traditional techniques. The meteorite was identified as a H5‐6 S4 W0 ordinary chondrite genomict breccia. The large amount of metal in the meteorite made a metallographic evaluation based on the opaque phases possible. The monocrystalline kamacite crystals suggest a higher petrological type and the distorted Neumann lines imply at least two different shock events. The absence of the plessite phase shows that the meteorite did not reach the highest shock levels S5 and S6. The well‐defined polycrystalline taenite is indicative of petrologic types 4 and 5 due to the conserved internal tetrataenite rim at the boundaries. The presence of polycrystalline taenites and the characteristics of the Agrell Effect suggest that the Santa Filomena meteorite did not reheat above 700°C. The absence of martensite confirms reheating temperatures <800°C and a slow cooling rate. The Ni contents and sizes of the zoned taenite particles indicate a slow cooling rate ranging from 1 to 10 K Myr−1.

МЕТЕОРИТНЫЕ ЭКСПЕДИЦИИ СОТРУДНИКОВ МУЗЕЯ ЗЕМЛЕВЕДЕНИЯ В 2022 Г

The paper briefly describes the results of the 2022 spring and summer search expeditions to the village of Tsarev, the Volgograd region (the meteorite shower “Tsarev”) and the Kamensk-Shakhtinsky district of the Rostov region (the Kamenskaya impact crater). The purpose of the expeditions was to search for and collect meteorites and impactites to replenish the exposition of the Earth Science Museum of Lomonosov Moscow State University with samples.

Minerochemical and Microtextural Study of the Ungrouped Iron Meteorite Oglat Sidi Ali, Eastern Highlands, Morocco, and Geomorphological Characterization of Its Strewnfield

Fragments of a new iron meteorite were found in and collected from Oglat Sidi Ali, Maatarka region, Morocco, during a series of expeditions in the years 2013–2017. The physical characteristics of recovered fragments feature typical attributes of individual samples of a unique meteorite strewnfield that originated from an iron meteorite shower via the fragmentation of a single body that broke up in the lower atmosphere. The total recovered mass of the Oglat Sidi Ali meteorite fragments was estimated to amount to more than 800 kg spread across a NE–SW oriented, 20 km-long and 5 km-wide strewnfield. Geochemical and mineralogical data achieved on Oglat Sidi Ali fragments, as well as the analysis of its microstructures obtained using electron backscattered diffraction (EBSD), suggested it should be classified as an ungrouped iron meteorite. A comparison of this meteorite with other ungrouped iron meteorites, such as NWA 859 and NWA 11010, purchased between 2001 and 2016 in various cities of Northeast Morocco show apparently similar mineralogy, geochemistry and textural features, suggesting a common origin from a single extraterrestrial body.

Metallographic Cooling Rate and Petrogenesis of the Recently Found Huoyanshan Iron Meteorite Shower

AbstractThe Huoyanshan iron meteorite shower, recently found in the Gobi Desert of Hami, Xinjiang, China, has very high Ni (21.1 wt%) content and low Au (2.0 ppm), Ir (0.02 ppm), Ge (1.7 ppm), and Ga (1.1 ppm) contents, and was classified into IAB‐sLH subgroup. The iron has a finest octahedrite structure of Widmanstätten pattern (the intergrowth of kamacite [α] and taenite [γ]) with plessite matrix, and euhedral schreibersite (Sch) crystals exclusively enclosed in kamacite bands. The textural features suggest the following formation process: γ→γ + Sch→γ + Sch + α, and then γ→α2 + γ. The metallographic cooling rate of Huoyanshan iron was determined to be 3–50°C/Myr using both the taenite Ni profile‐matching and taenite central Ni content methods, with the bandwidths corrected for crystallographic orientation by electron backscatter diffraction (EBSD). The cooling rate of Huoyanshan is consistent with other sLH irons and confirms the slow cooling history of the IAB low‐Au subgroups. These slow cooling rates require immediate re‐accretion with a thick brecciated fragments layer in the parent body after the impact melting event. The depleted but unfractionated Re, Os, Ir, Ru, and Pt and the enriched Pd and Au abundances of Huoyanshan iron and other sLH subgroup irons show complementary feature to that of refractory metal nuggets in Ca‐, Al‐rich inclusions (CAIs), which could be explained by extracting the metallic Fe‐Ni with HSE predominantly remained in CAIs from a CAI‐bearing asteroid. The very high Ni content of sLH subgroup and its Mo isotope evidence (Worsham et al., 2017, https://doi.org/10.1016/j.epsl.2017.02.044) suggest it has an oxidized parent body with non‐carbonaceous chondrite‐like precursor composition. We propose that the sLH subgroup was produced by impact melting of a LL like and CAI‐bearing asteroid, followed by fast burying of thick and porous silicate breccia.

Neutron capture 128Xe and 129Xe in the San Juan mass of the Campo del Cielo IAB iron meteorite: Evidence for a high fluence of thermalized neutrons

AbstractThe petrographic study of the San Juan A2 polished section demonstrated textural and compositional similarities with the Campo del Cielo IAB iron meteorite, with trace element abundances in metal following the pattern of bulk Campo del Cielo. Xenon, neon, and helium isotopic compositions have been measured in radial graphite rims, massive graphite inclusions, fine‐grained graphite aggregates, cliftonite, and platy graphite. Two silicate inclusions and two areas of metal were also analyzed. 3He/4He versus 4He/21Ne data for San Juan metal plot next to the values reported for the El Taco fragment of Campo del Cielo, supporting San Juan being a part of the Campo del Cielo meteorite shower. Based on the Ne isotopic composition of its components, and the observed correlation between 128Xe and 129Xe, the San Juan A fragment of Campo del Cielo was well shielded from the primary galactic cosmic ray high‐energy irradiation. Its size allowed the secondary neutrons to be fairly well thermalized, receiving an equivalent (normalized to the research reactor with highly thermalized neutron spectrum) fluence of thermal and epithermal neutrons of 6.6 × 1017 n cm−2. Considering 1.8 × 108 years single‐stage and constant exposure geometry irradiation history for Campo del Cielo, and assuming the identical neutron flux spectra for the research reactor and Campo del Cielo, the average thermal equivalent neutron flux for San Juan is about 1.2 × 102 n cm−2 s−1. Xe isotopic composition in the radial graphite rims and platy graphite shows evidence of live 129I in San Juan and is consistent with a mixture of iodine‐derived and tellurium‐derived Xe.

The Kumtag meteorite strewn field

The Kumtag meteorite strewn field was found in the Kumtag desert, 132 km south of Hami city in the Xinjiang province, China. It is an ellipse of 2.5 × 7.9 km, with a long axis extending along the northeast-southwest direction. The largest individual meteorite of the strewn field weighs about 10 kg; the smallest individual has a mass of only 27 g. In total, more than 100 individuals with a total mass of more than 180 kg were collected. The location and the distribution of the fragments suggest that the Kumtag meteoroid entered the atmosphere in the direction Northeast-Southwest. All meteorites collected in this strewn field are samples from the same unique meteorite shower. The Kumtag meteorite is an H5 ordinary chondrite with a shock stage S2, and a weathering grade W2. The cosmic ray exposure age of Kumtag is 6.7 ± 0.8 Ma, which is rather typical for H chondrites and which indicates that Kumtag was derived from the massive impact event on its parent body ~7 Ma ago. A significant amount of He has been lost during certain unknown processe(s) before the Kumtag meteorite was ejected from its parent body.

The Santa Rosa de Viterbo meteorite, Colombia. New work on it's petrological, geochemical and economical characterization

Undifferentiated meteorites, like primitive chondrites, can contain presolar and solar nebula materials which would provide information about the origin and initial conditions of the solar system, whereas differentiated meteorites like iron meteorites, can show early phases of planetary accretion. They also provide the possibility to receive information about core properties and planetary bodies. In addition to the gain in such fundamental scientific knowledge both types are of interest for the exploration of critical raw materials (CRMs) and precious elements.The Santa Rosa de Viterbo meteorite shower, discovered 1810 in the Boyacá province of Colombia, represents a typical iron-nickel meteorite. The present study presents new structural, textural and geochemical results of one fragment of this meteorite, using reflecting microscopy, electron probe micro analyses (EPMA) and electron microscopy (SEM) with energy dispersive X-ray spectroscopy (EDX). The present study presents trace element concentrations of the meteorite's minerals for the first time.The sample is dominated by kamacite (α-FeNi). Schreibersite (FeNi3P), taenite (γ-FeNi) and plessite (mixture of kamacite and taenite) are minor constituents. The occurrence of cohenite ((Fe,Ni,Co)3C) and troilite (FeS) are likely. The meteorite sample contains classical Neuman bands passing through kamacite and frequent Widmanstätten pattern. The bandwidth of kamacite defines the meteorite as finest octahedrite. Geochemically, it is characterized as a “Type IC meteorite”.While improving the characterization and classification of the Santa Rosa de Viterbo Iron Meteorite, notable concentrations of Au (>400 ppm) and Ge (>230 ppm) alongside major elements such as Fe, Ni and Co in the bulk composition of that meteorite, were proven. Major and rock-forming minerals such as kamacite and taenite incorporate hundreds of ppm of Ge whereas schreibersite, itself a minor component in that particular meteorite, is the major source for Au (>1400 ppm). In kamacite and taenite also Ir, Pd and Ga were found in minor amounts. Nano-scale inclusions or atomic clusters called nano-nuggets may have been responsible for the high concentrations of Au, Ir, Pd and Ga. Raman and Laser-induced plasma spectroscopes installed in in space probes seems suitable exploration methods for Fe–Ni meteorites, containing Ni-concentrations > 5.8 wt% defining the meteorite as octaedrites.

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.

El condrito carbonáceo Aguas Zarcas: bólido, caída y recuperación de un meteorito extraordinario del tipo CM2

On April 23rd, 2019 at 21:08 local time, a fireball was observed crossing the night sky of central Costa Rica with a general southeast to northwest direction, in an event registered by both witnesses and cameras. A subsequent explosive sound (fragmentation in the atmosphere) was reported near San Carlos, followed by a meteorite shower in the districts of Aguas Zarcas and La Palmera, of San Carlos. The first recovered fragment (1071 g) came from a house near La Caporal in Aguas Zarcas, where the impact bored a hole in the ceiling breaking the meteorite in smaller pieces adding up to a total weight of 1152 g. In the following days several other fragments were recovered towards the northwest of Aguas Zarcas, in the towns of La Cocaleca, Santa Rosa, and La Palmera, with weights ranging from <1g to 1875 g. The total recovered mass of the meteorite was estimated in roughly 30 kg. After proper revision by the Meteoritical Society, the official name “Aguas Zarcas Meteorite” was approved on May 30th, 2019. The main masses of the meteorite, in excess of ~50 g, show regmaglypts (some with iridescent surfaces). Other fragments display drop, platy, and elliptical forms, with aerodynamic patterns, and showing a frontal dome. The inner parts of the analyzed specimens show chondrules on varying areal percentages, within a dark-gray to black matrix. Calcium-Aluminum rich inclusions (CAI), sub-millimetric crystals of plagioclase, olivine, and sulphide and metallic flakes are also present in the matrix. A clear fusion crust is evident in some fragments showing cooling microfractures. It is slightly magnetic and expels a particular organic-like odor. Geochemical and isotopic analyses performed at the Universities of Costa Rica, Arizona and Nuevo Mexico, among others, and the observed textural characteristics of the meteorite, indicate that it belongs to the Carbonaceous Chondrite classification of rocky meteorites, type CM2 which entails the presence of hydrated minerals within a fine matrix composed of carbon, and nickel-rich sulphides components. CM2 meteorites also show general compositions and oxygen isotope compositions similar to the primitive solar nebula. Carbonaceous chondrites represent only ~4% of the total recovered meteorites worldwide and they preserve the geochemical, isotopic, and mineralogical composition of the first millions of years of the history and evolution of the Solar System, making the Aguas Zarcas Meteorite an extraordinary event, and sparking national and international scientific interest.

Joshua’s Celestial Miracle was not an Eclipse: the Long and the Short

Humphreys & Waddington have recently suggested that the Biblical account involving Joshua’s control of the sun and moon (Joshua 10. 1-15) was inspired by an annular eclipse. Going by the text as given, it is shown that the explanation as an eclipse, whether annular or total, is unacceptable on calendrical, philological and physical grounds alike. The story’s possible historicity cannot be properly evaluated until it is placed in two cross-cultural and sometimes overlapping contexts: ritual utterances before battle designed to divine the outcome or provoke divine intervention in it and the mythology of solar arrests, reversals and radical alterations of the length of day. ‘Solar magic’ emerges as a common archaic practice in real life as well as legend. Some literary parallels are cited which have never before been linked with Joshua. All things considered, the tale may have originated as an embellished memory of some extraordinary natural event other than an eclipse, coinciding with a historical battle. A tempting possibility is the aerial passage of a fragmenting bolide, producing a meteorite shower and nocturnal illumination.

Joshua’s Celestial Miracle was not an Eclipse: the Long and the Short

Humphreys &amp; Waddington have recently suggested that the Biblical account involving Joshua’s control of the sun and moon (Joshua 10. 1-15) was inspired by an annular eclipse. Going by the text as given, it is shown that the explanation as an eclipse, whether annular or total, is unacceptable on calendrical, philological and physical grounds alike. The story’s possible historicity cannot be properly evaluated until it is placed in two cross-cultural and sometimes overlapping contexts: ritual utterances before battle designed to divine the outcome or provoke divine intervention in it and the mythology of solar arrests, reversals and radical alterations of the length of day. ‘Solar magic’ emerges as a common archaic practice in real life as well as legend. Some literary parallels are cited which have never before been linked with Joshua. All things considered, the tale may have originated as an embellished memory of some extraordinary natural event other than an eclipse, coinciding with a historical battle. A tempting possibility is the aerial passage of a fragmenting bolide, producing a meteorite shower and nocturnal illumination.

The Sariçiçek howardite fall in Turkey: Source crater of HED meteorites on Vesta and impact risk of Vestoids

AbstractThe Sariçiçek howardite meteorite shower consisting of 343 documented stones occurred on September 2, 2015 in Turkey and is the first documented howardite fall. Cosmogenic isotopes show that Sariçiçek experienced a complex cosmic‐ray exposure history, exposed during ~12–14 Ma in a regolith near the surface of a parent asteroid, and that an ~1 m sized meteoroid was launched by an impact 22 ± 2 Ma ago to Earth (as did one‐third of all HED meteorites). SIMS dating of zircon and baddeleyite yielded 4550.4 ± 2.5 Ma and 4553 ± 8.8 Ma crystallization ages for the basaltic magma clasts. The apatite U‐Pb age of 4525 ± 17 Ma, K‐Ar age of ~3.9 Ga, and the U,Th‐He ages of 1.8 ± 0.7 and 2.6 ± 0.3 Ga are interpreted to represent thermal metamorphic and impact‐related resetting ages, respectively. Petrographic; geochemical; and O‐, Cr‐, and Ti‐isotopic studies confirm that Sariçiçek belongs to the normal clan of HED meteorites. Petrographic observations and analysis of organic material indicate a small portion of carbonaceous chondrite material in the Sariçiçek regolith and organic contamination of the meteorite after a few days on soil. Video observations of the fall show an atmospheric entry at 17.3 ± 0.8 km s−1 from NW; fragmentations at 37, 33, 31, and 27 km altitude; and provide a pre‐atmospheric orbit that is the first dynamical link between the normal HED meteorite clan and the inner Main Belt. Spectral data indicate the similarity of Sariçiçek with the Vesta asteroid family (V‐class) spectra, a group of asteroids stretching to delivery resonances, which includes (4) Vesta. Dynamical modeling of meteoroid delivery to Earth shows that the complete disruption of a ~1 km sized Vesta family asteroid or a ~10 km sized impact crater on Vesta is required to provide sufficient meteoroids ≤4 m in size to account for the influx of meteorites from this HED clan. The 16.7 km diameter Antionia impact crater on Vesta was formed on terrain of the same age as given by the 4He retention age of Sariçiçek. Lunar scaling for crater production to crater counts of its ejecta blanket show it was formed ~22 Ma ago.

Effects of Rayleigh-Taylor instability and ionospheric plasma bubbles on the global navigation satellite System signal

Ionospheric disturbances induced by various natural (e.g., earthquakes, volcanic eruption, thunderstorms, meteorite showers, solar eclipses) or anthropogenic (e.g., nuclear explosions, launching of space shuttles) processes can be detected through change in Total Electron Content (TEC) in the F-layer. These ionospheric perturbations can be captured by worldwide expanding geodetic (GNSS) networks, mainly during the day time, when the solar radiation ionizes the air molecules. However, during post-sunset period, strong ionospheric irregularities (known as Equatorial Plasma Bubbles, EPBs) develop due to the classical configuration for the Rayleigh-Taylor (R-T) instability that diffracts navigation and communication signals. Here we use various instances of ionospheric disturbances triggered by natural processes (e.g., earthquakes and volcanic eruption), in the recent decade to investigate the spatiotemporal and seasonal effects of ionospheric irregularities on the GNSS signals. Our study suggests that in the low-latitudinal region (e.g., Sumatra, Mexico), such ionospheric irregularities can mask the ionospheric perturbations due to the higher production rate of EPBs. Hence detection of such co-seismic TEC anomaly becomes difficult. However, in the high-latitudinal region (e.g., Iceland, Alaska), due to the lower production rate of EPBs, ambient ionospheric irregularities are insignificant and hence coseismic TEC anomalies can be captured even during night time. We argue that the production rate of EPBs further depends upon seasonal and longitudinal parameters on the globe.

New insights on the Dronino iron meteorite by double-pulse micro-Laser-Induced Breakdown Spectroscopy

Two fragments of an iron meteorite shower named Dronino were characterized by a novel technique, i.e. Double-Pulse micro-Laser Induced Breakdown Spectroscopy (DP-μLIBS) combined with optical microscope. This technique allowed to perform a fast and detailed analysis of the chemical composition of the fragments and permitted to determine their composition, the alteration state differences and the cooling rate of the meteorite. Qualitative analysis indicated the presence of Fe, Ni and Co in both fragments, whereas the elements Al, Ca, Mg, Si and, for the first time Li, were detected only in one fragment and were related to its post-falling alteration and contamination by weathering processes. Quantitative analysis data obtained using the calibration-free (CF) - LIBS method showed a good agreement with those obtained by traditional methods generally applied to meteorite analysis, i.e. Electron Dispersion Spectroscopy - Scanning Electron Microscopy (EDS-SEM), also performed in this study, and Electron Probe Microanalysis (EMPA) (literature data). The local and coupled variability of Ni and Co (increase of Ni and decrease of Co) determined for the unaltered portions exhibiting plessite texture, suggested the occurrence of solid state diffusion processes under a slow cooling rate for the Dronino meteorite.

Main parameters of meteoroid motion during the fall of the Chelyabinsk meteorite shower on February 15, 2013

A rapid method is proposed for determining a meteoroid’s trajectory in the Earth’s atmosphere and its height and velocity at individual points. The method is designed for use with video material (regardless of the motion speed of the video recorder) for daytime bolide events. Kinematic parameters are obtained for the superbolide event followed by the Chelyabinsk meteorite shower on February 15, 2013. The (geodetic) azimuth of the meteoroid’s trajectory in the Earth’s atmosphere is 283.39° ± 1.7° (or 101.09° ± 1.7° toward the radiant). The radiant altitude over the site with observations of the end of the first fragmentation phase is 20.5°. The geodetic coordinates of the beginning of the bolide phenomenon and the point of suspension of the radiating material at the end of the first fragmentation phase are (64°00′02.74″ ± 2.1′ east longitude; 54°30′54.66″ ± 3.0′ north latitude) and (61°11′01.88″ ± 1.6′ east longitude; 54°52′06.68″ ± 3.1′ north latitude), respectively. The atmospheric entry velocity is 19.29 ± 0.89 km s−1. The height of the start of the light emission is 102.4 km; those of the main fragmentation phases are 28.0 and 24.4 km. The calculated elements for the heliocentric orbit of the Chelyabinsk meteoroid are: Q = 2.66 ± 1.20 AU, q = 0.73 ± 0.01 AU, a = 1.67 ± 0.10 AU, e = 0.57 ± 0.03, i = 7.07° ± 0.54°, Ω = 326.42°, and ω = 106.28° ± 2.54°. These parameters are compared with the results obtained by other authors.

Critical core mass for enriched envelopes: the role of H2O condensation

Context. Within the core accretion scenario of planetary formation, most simulations performed so far always assume the accreting envelope to have a solar composition. From the study of meteorite showers on Earth and numerical simulations, we know that planetesimals must undergo thermal ablation and disruption when crossing a protoplanetary envelope. Once the protoplanet has acquired an atmosphere, the primordial envelope gets enriched in volatiles and silicates from the planetesimals. This change of envelope composition during the formation can have a significant effect in the final atmospheric composition and on the formation timescale of giant planets. Aims. To investigate the physical implications of considering the envelope enrichment of protoplanets due to the disruption of icy planetesimals during their way to the core. Particular focus is placed on the effect on the critical core mass for envelopes where condensation of water can occur. Methods. Internal structure models are numerically solved with the implementation of updated opacities for all ranges of metallicities and the software CEA to compute the equation of state. CEA computes the chemical equilibrium for an arbitrary mixture of gases and allows the condensation of some species, including water. This means that the latent heat of phase transitions is consistently incorporated in the total energy budget. Results. The critical core mass is found to decrease significantly when an enriched envelope composition is considered in the internal structure equations. A particular strong reduction of the critical core mass is obtained for planets whose envelope metallicity is larger than Z=0.45 when the outer boundary conditions are suitable for condensation of water to occur in the top layers of the atmosphere. We show that this effect is qualitatively preserved when the atmosphere is out of chemical equilibrium.

Density, porosity and magnetic susceptibility of the Košice meteorite shower and homogeneity of its parent meteoroid

Bulk and grain densities, porosities, and magnetic susceptibilities of 67 individuals of Košice H chondrite fall were measured. The mean bulk and grain densities were determined to be 3.43g/cm3 with standard deviation (s.d.) of 0.11g/cm3 and 3.79g/cm3 with s.d. 0.07g/cm3, respectively. Porosity is in the range from 4.2% to 16.1%. The logarithm of the apparent magnetic susceptibility (in 10−9m3/kg) shows narrow distribution from 5.17 to 5.49 with mean value at 5.35 with s.d. 0.08.These results indicate that all studied Košice meteorites are of the same composition down to ~g scale without the presence of foreign (non-H) clasts and are similar to other H chondrites. Košice is thus a homogeneous meteorite fall derived from a homogeneous meteoroid.

Fragments of the Chelyabinsk meteorite shower: Distribution of masses and sizes and constraints on the mass of the largest fragment

This paper reports data on the masses of fragments of the Chelyabinsk meteorite shower (fall of 15.02.2013). Assuming a lognormal distribution for the masses of fragments, the logarithm of the mean mass and standard deviation were estimated for the available data, describing the distribution density of masses and calculated diameters of fragments. Based on the dependence of the cumulative number of fragments with masses equal or greater than a given value, the mass of the largest fragment of the Chelyabinsk meteorite shower was estimated. It was shown that the most probable mass of such a fragment is hundreds of kilograms for a total mass of infalling material of 100 metric tons (t) and 1–2 t for a total mass of 1000 t, and the lower constraint for the maximum mass of the fragment is a few tens of kilograms.

Katol Meteorite Shower, Maharashtra: A Preliminary Study

Abstract: A meteorite shower occurred in Katol (21° 15' 30" N ; 78° 35' 00" E ; at an elevation of 415 m above msl), Nagpur district of Maharashtra state, India on May 22, 2012 between 14:00 to 14:30 hrs (Indian Standard Time) with a presently observed strewn field of ~5.0 sq km area. The event was experienced by the hundreds of inhabitants with a loud noise and fire ball between Akola in the west to Nagpur in the east. The Geological Survey of India has so far collected 27 meteorite pieces with a total weight of 3500 gm. The locations, size, shape and surface features of the individual meteorite pieces have been recorded. Based on their physical properties, mineralogy, mineral chemical mapping and REE chemistry, the Katol meteorites have been classified as olivine-rich H5 type differentiated stony meteorite with reconstituted chondrules. The preliminary evidence suggests the presence of pre-solar grains in Katol meteorite.

Ablation spherules in the Sikhote Alin meteorite and their genesis

Practically all of the examined spherules extracted in 1948–1949 from soil at the crater field of the 1947 Sikhote Alin meteorite shower are ablation spherules produced during this meteorite fall. The spherules can classified into two textural types: (i) fine-grained, which consist of Ni-bearing magnetite (3–6 wt % NiO) dendrites, sometimes with minor amounts of interstitial P- and Fe-rich material, and (ii) coarse-grained, which also consist of Ni-bearing magnetite dendrites or grains, sometimes with wuestite, an interstitial material, which resembles that in type (i) or has a silicate composition. The texture, mineralogy, and chemistry (presence of P and Si) of these spherules differ from those of iron cosmic spherules (type I) that occur in the background flux of micrometeorites. The spherules are thought to were produced by the ablation of meteoritic material at elevations of about 12 km (in the region where disintegration starts) and below, at maximum temperatures of 1600–2180°C and oxygen fugacity of 10−14 to 10−1 atm. Conceivably, the ablated material was enriched in silicates compared to the fallen material.