Wyniki wyszukiwania - Biblioteka Nauki

1

The extraterrestrial matter falls in west-central Poland (Great Poland Lowland); historical and geological data

100%

Stankowski W. T. J.

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tom Vol. 65, no. 2

263--268

EN

Direct and indirect evidence of falls of extraterrestrial matter in west-central Poland (Great Poland Lowland) is proved historically and environmentally. The chronological list of such events has historical (documents, medieval paintings, newspaper reports), geological and morphological documentation. The most important are the environmental sites of Morasko/Oborniki, Przełazy and Jankowo Dolne, where metallic meteorites were recognized. These meteorite falls represent a series of cosmic events: the Morasko fall was c. 5000 years BP, the Przełazy fall was c. 10000 years BP, and the age of the Jankowo Dolne fall is not fully documented.

2

First chemical characterization of the new Polish meteorite "Baszkówka" by neutron activation analysis

86%

Dybczyński R. , Danko B. , Kulisa K. , Polkowska-Motrenko H. , Samczyński Z. , Stępniewski M. , Szopa Z.

Chemia Analityczna

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1999

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tom Vol. 44, No. 3A

471-484

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Wyniki badań mineralogicznych i petrologicznych nowych okazów meteorytu Pułtusk w 150 rocznicę spadku

72%

Przylibski T. A. , Łuszczek K.

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tom Vol. 66, nr 6

368--378

EN

One of the largest observed stone meteorite shower in the history of mankind on Earth took place on Thursday evening on January 30, 1868, about seven o’clock near Pułtusk in Poland. Despite the 150th anniversary of the fall of chondrite officially classified as Pułtusk H5 with a shock stage S3 there is still little published data on the chemical composition of minerals of this chondrite as well as its petrological characteristics in the literature. The authors carried out mineralogical and petrological research that will help a little to fill this gap in knowledge about the Pułtusk chondrite. Meteorite specimens found by Piotr Kuś in 2015 and investigated by the authors are undoubtedly part of the Pułtusk fall of January 30, 1868. They can be classified as ordinary chondrite H5, S2,W2. The authors stated that the studied rock is characterized by a varied shock level -from S1 to S2/3, as well as it contains chondrules of the chromite-plagioclase unequilibrated rock. In the composition of the examined fragment of Pułtusk chondrite, the authors identified silicates: olivine, diopside, bronzite and clinohyperstene, and oligoclase, oxides: chromite (and spinel), sulfides: troilite, FeNi alloy mineral phases: kamacite and taenite, as well as phosphates: merrilite and apatite. The chemical composition of olivine crystals as well as low- and high-Ca pyroxenes crystals and plagioclase crystals (about the composition of oligoclase) confirms that the examined specimen comes from the Pułtusk fall and it is a rock that should be classified as a petrographic type H5.

4

Charakterystyka petrograficzna skał pochodzących ze struktury impaktowej Gardnos, Norwegia

72%

Jarmołowicz-Szulc K. , Ilcewicz-Stefaniuk D. , Stefaniuk M.

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tom nr 464

43--48

PL

Krater meteorytu Gardnos znajduje się w Norwegii, ok. 125 km na północny zachód od Oslo. Cała struktura jest dobrze widoczna w terenie dzięki licznym odkrywkom brekcji impaktowych i utworów poimpaktowych występujących w okręgu o promieniu ok. 5 km. Główne typy skał impaktowych w rejonie krateru Gardnos to autochtoniczna brekcja z Gardnos oraz przykrywająca ją allochtoniczna brekcja impaktowa (suevit). W artykule omówiono petrografię tych skał. Brekcja z Gardnos jest brekcją lityczną, złożoną ze spękanych fragmentów skał, ale nie zawiera fragmentów stopu. Suevit jest brekcją polimiktyczną, zawierającą małe fragmenty zrekrystalizowanego stopu z klastami skał i minerałów.

EN

The crater of the Gardnos meteorite is located in Norway, about 125 km north-west of Oslo. The structure is well seen due to the outcrops of impact breccias and post-impact deposits that form a circle with a radius of about 5 km. Main types of the impact rocks in the Gardnos area are the autochthonous Gardnos breccia and its cover – allochthonous suevite breccia. The petrological characteristics of these rocks are presented. The Gardnos breccia is a lithic breccia, composed of fissured rock fragments, without melt components. The suevite is a polymictic breccia, built of small fragments composed of recrystallized melt and clasts of rocks and minerals.

5

Different diamonds in meteorites - DaG 868 and NWA 3140 ureilites

72%

Karczemska A. , Jakubowski T. , Vergas F.

Journal of Achievements in Materials and Manufacturing Engineering

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2009

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tom Vol. 37, nr 2

292-297

EN

Purpose: Ureilites are a rare type of meteorites containing tiny diamond grains. In our research we used two ureilites: NWA 3140 and DaG 868. The aim of this paper is to show the non-uniformity of carbon in ureilites, especially differences of ureilitic diamonds. Design/methodology/approach: One of the best methods to examine different allotropic forms of carbon is Raman Spectroscopy. This method used to investigate diamonds provides a lot of information about diamond polytypes, crystals sizes, a level of defects and internal stresses, etc. 2D imaging was done with a Confocal Raman Imaging alpha 300 R WITec apparatus equipped with an Nd:YAG laser with 532 nm excitation. The spectra were collected with a high-sensitive confocal microscope connected to a high-throughput spectrometer equipped with a CCD camera. Mean and local elemental compositions of the samples were determined by an energy dispersive X-ray (EDX) method. A scanning electron microscope HITACHI S-3000 N was used to characterize microstructures (carbon veins) of the samples. Findings: Different diamond generations were found in ureilites in the presented research with a wide range of Raman shifts from 1309 cm -1 to 1339 cm -1. Also graphite and amorphous carbon were found. Research limitations/implications: Presented research is another step to solve the problem about diamond origin in meteorites. Practical implications: Understending diamonds and the other carbon phases in meteortites could help in manufacturing new carbon materials in laboratory. Originality/value: Authors use Raman imaging to show distribution of diamonds in ureilites, this is pioneer research, results of DaG 868 and NWA 3140 are shown for the first time.

6

The investigation of genetic relationship between the Baszkówka and Mt. Tazerzait chondrites by NAA and other methods

72%

Dybczyński R. , Borucki J. , Danko B. , Kulisa K. , Polkowska-Motrenko H. , Samczyński Z. , Stępniewski M. , Szopa Z. , Tanida K.

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tom Vol. 46, No. 4

477-488

EN

The similarity of two meteorites, Baszkowka (Poland, 1994) and Mt. Tazerzait (Niger, 1991), was studied by instrumental and radiochemical neutron activation analysis supplemented by mercury determination with the aid of an automatic mercury analyzer yielding data for 23 elements. The bulk composition of both meteorites is nearly identical within the experimental error. Their composition is also similar to the mean composition of L chondrites but there are marked deviations in the cases of Pd, Os, Pt, Cu and Hg. It seems also that both meteorities are slightly enriched in light rare earth elements (REE) and slightly depleted in heavy REE in comparison with L chondrites. This study supports earlier suggestions based on petrological properties, abundance of noble gases and their isotopic composition, gas retention ages and cosmic ray exposure ages, that these two chondrites have the same origin and the common parent body. It cannot be excluded that this parent body is different from that typical for all other known L chondrites.

PL

Stosując instrumentalną i radiochemiczną neutronową analizę aktywacyjną oraz automatyczny analizator rtęci badano podobieństwo dwóch meteorytów o nazwach: Basz-kówka (Polska, 1994) oraz Mt. Tazerzait (Niger, 1991). Na podstawie oznaczenia 23 pierwiastków stwierdzono, że całościowy skład obu meteorytów jest niemal identyczny w granicach błędu doświadczalnego. Ich skład jest też podobny do średniego składu chondrytów typu L, jednakże z istotnymi odchyleniami w przypadku Pd, Os, Pt, Cu i Hg. Wydaje się także, że oba meteoryty są nieznacznie wzbogacone w lekkie i nieznacznie zubożone w ciężkie ziemie rzadkie w stosunku do chondrytów L. Badania te potwier-dzająwcześniejsze sugestie, oparte na własnościach petrologicznych, obecności gazów szlachetnych i ich składu izotopowego, wieku zatrzymania gazu oraz wieku kosmicznego napromieniowania że oba chondryty mają takie samo pochodzenie i wspólne ciało macierzyste. Nie jest wykluczone, że to ciało macierzyste różni się od ciała macierzystego wszystkich innych chondrytów typu L.

7

Meteoryty, kratery uderzeniowe i inne ślady kosmicznej katastrofy w rejonie Moraska pod Poznaniem

72%

Szczuciński W. , Muszyński A.

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2020

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tom Vol. 68, Nr 8

637--644

EN

About 5,000 years ago near Morasko (the district of the present-day city of Poznań, western Poland) the largest known iron meteorite shower in Central Europe took place. The evidence of that impact, documented so far, comprises numerous iron meteorite fragments distributed over an area of approximately 3 km2 and at least six meteorite impact craters with a maximum diameter of about 100 m. The present paper reviews the most recent findings related to the meteorite, craters, processes of their formation, as well as the environmental effects of the impact in the Morasko area. The most important findings, reported in this review cover: 1) the recognition of two new minerals in the meteorite: moraskoite and czochralskiite; 2) the identification and detailed analysis of the ejecta layer around the craters and underlying paleosoil providing evidence for the mid-Holocene age of the impact; 3) the numerical modelling constraining the range of likely physical properties of the impactor, e.g. the diameter of the projectile forming the largest crater and its landing velocity (c. 1.5 m and 10km/s, respectively);4) the studies of the nearby lake and peat deposits revealing restricted environmental effects of the impact. The Morasko craters field is currently one of the best-studied examples of small/moderate-sized meteorite impact in unconsolidated sediments.

8

Chondryt Antonin – pierwszy polski meteoryt ze zrekonstruowaną orbitą wokółsłoneczną. Raport z klasyfikacji i rejestracji oraz propozycje działań mogących wzbogacić kolekcję polskich meteorytów

72%

Krzesińska A. , Tymiński Z. , Maćkowska R.

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tom Vol. 71, nr 7

372--385

EN

On July 15, 2021, a bright fireball was registered over Poland and it led to a meteorite fall near the towns of Antonin and Mikstat, on the border of the Greater Poland and Lower Silesia voivodeships. Soon after registration of the bolide, a meteorite fragment was found. Observation of the fireball's trajectory helped to reconstruct the pre-atmospheric parameters of the meteoroid, such as the orbit inclination or eccentricity (Shrbený et al., 2022). Additionally, finding of the meteorite fragment enabled petrographic research and reconstruction of the thermal and collisional history of meteorite'sparent body. The Antonin meteorite is the first Polish meteorite with the reconstructed pre-atmospheric orbit and, atthe moment, one of only fifty in theworld. It is an L5 ordinary chondrite (Shrbený et al., 2022; Krzesińska, 2023). Here we present a report on the classification and registration process of the Antonin meteorite. Registration included measurements of cosmogenic isotope, necessary to prove the connection of the meteorite with the observed bolide. The specimen was found during the private expedition, so no direct proof existed for find in the predicted fall area. Cosmogenic isotope study allowed to assessing the time of meteorite fall, which matched the fireball event. Classification included petrographic and mineralogical analysis of the rock. The fall and find circumstances of Antonin allowed us to reflect on the lack of awareness of the Polish society regarding meteorites. Such unawareness is also seen when the whole collection of Polish meteorites is statistically analysed. We present such analysis at the end of the paper, and conclude that many meteorite falls in Poland must be unnoticed. Additionally, inability of citizens to recognize a meteorite, especially a chondrite, causes that many of these rocks remain unrecovered. The aim of this paper is to inspire the reader to pay attention to falls of meteorites, and to look for potential meteorite rocks. In final, we encourage the readers to get involved in activities of fireball networks and to take part in meteorite recovery trips.

9

Diamonds in ureilites

72%

Jakubowski T. , Karczemska A. , Kozanecki M.

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tom Vol. 0, No. 0

3-8

EN

The presence of diamonds in meteorites was confirmed for the first time in the Novo-Ureiureilite in 1888. Ureilites are a rare class of achondrites, often referred to as primitive achondrites. They are composed of olivine and pyroxene (pygeonite), as well as graphite inclusions often coexisting with diamonds. The following three main hypotheses of diamond origin in ureilites have been proposed: the HPHT process, graphite-to-diamond conversion under shock compression due to impact on the parent body (the most popular theory, as of the time of publication), and the CVD process in the solar nebula. The samples of all types of ureilites, from less shocked up to highly shocked, were examined using Raman Spectroscopy and Scanning Electron Microscopy. The results show the presence of diamonds in all of our samples. Of particular significance is the comparison of Raman spectra of diamonds and graphite phases of different ureilites.

10

Nanometer-sized mineral grains and their genetic types in meteorites

72%

Semenenko V. P. , Girich A. L. , Shkurenko K. O. , Kychan N. V. , Shyrinbekova S. N. , Gorovenko T. M.

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tom Vol. 1, No. 1

13-19

EN

Three genetically different types of nanometer-sized mineral grains in meteorites can be distinguished based on literature and original data: (a) primitive condensates, (b) metamorphic grains, and (c) weathering products. The first of these groups were formed by condensation in a gas-dust nebula in either a presolar or solar environment. Metamorphic grains were formed as a result of thermal, shock or aqueous metamorphism on the meteorite parent bodies. The third type can clearly be characterized as terrestrial weathering products, which are generally found in meteorite finds and are rare or absent within meteorites recovered shortly after having fallen. Nanometric components are found predominantly within the fine-grained silicate material of primitive meteorites. It is suggested that enhanced accretional properties of nanometer-sized grains could be responsible for the primary accretion of condensed nanoglobules within a protoplanetary nebula. The nature of nanometer-sized inclusions of native W and native Ag originally discovered in the Krymka chondrite is preliminarily discussed.

11

Chondryty węgliste CI oraz podobne do CI

72%

Blutstein K.

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tom 15

7-26

PL

Chondryty węgliste z grupy CI stanowią najbardziej pierwotną materię w Układzie Słonecznym dostępną do badań. Obecnie tylko 9 meteorytów zostało sklasyfikowanych jako chondryty węgliste grupy CI, z czego dla dwóch z nich klasyfikacja ta jest kwestionowana. W literaturze sugeruje się, aby te dwa meteoryty, wraz z innymi podobnymi, uznać za osobną grupę CY. Dodatkowo, meteoryt Tagish Lake jest rozważany jako CI2, chociaż ta klasyfikacja nie zdobyła powszechnej akceptacji. Na podstawie ograniczonej ilości źródeł literaturowych dotyczących składu pierwiastkowego chondrytów grupy CI oraz chondrytów podobnych do CI, stwierdzono, że chondryty Alais, Ivuna oraz Orgueil mają najbardziej zbliżony skład pierwiastkowy. Skład chondrytu Tonk różni się nieznacznie, ale wciąż mieści się w zakresie typowym dla chondrytów grupy CI. Skład chemiczny meteorytu Revelstoke znacząco odbiega od średniego składu chondrytów grupy CI, jednak niewielka masa tego meteorytu (1 g) i brak dostatecznej ilości danych mogą wpływać na wyniki. Spośród chondrytów podobnych do CI, najlepsze dopasowanie składu chemicznego do grupy CI wykazuje chondryt Tagish Lake. Natomiast najgorsze dopasowanie charakteryzuje chondryt Belgica 7904, uważany za członka potencjalnej grupy CY, jednak na podstawie składu chemicznego jednoznacznie można stwierdzić, że nie należy do grupy CI lub CY. Chociaż potencjalne chondryty CY wykazują znaczne zubożenie w kadm, nie można wykluczyć przypadkowej zbieżności w tej kwestii. Z perspektywy górniczej, ciała macierzyste chondrytów węglistych grupy CI mogą stanowić potencjalne źródło wody, a co za tym idzie, również wodoru, mającego istotne znaczenie jako potencjalne paliwo. Planetoida 1508 Kemi będąca potencjalnym ciałem macierzystym chondrytów węglistych grupy CI może zawierać około 3,39·1012 Mg wody, w tym około 3,76·1011 Mg wodoru.

EN

Carbonaceous chondrites of the CI group represent the most primitive matter in the Solar System available for study. Currently, only 9 meteorites have been classified as CI group carbonaceous chondrites, with the classification of two of them being questioned. In the literature, there is a suggestion to consider these two meteorites, along with others that share similarities, as a separate CY group. Additionally, the Tagish Lake meteorite is considered CI2, although this classification has not gained widespread acceptance. Based on a limited number of scientific sources regarding the elemental composition of CI group carbonaceous chondrites and CI-like chondrites, it has been observed that Alais, Ivuna, and Orgueil chondrites have the most similar elemental composition. The composition of the Tonk chondrite differs slightly but still falls within the typical range for CI group chondrites. The chemical composition of the Revelstoke meteorite significantly deviates from the average composition of CI group chondrites; however, the small mass of this meteorite (1 g) and a lack of sufficient data may affect the results. Among CI-like chondrites, the best match in chemical composition to CI chondrites is found for the Tagish Lake chondrite. Conversely, the Belgica 7904 chondrite, previously considered a member of the potential CY group, unequivocally does not belong to CI or CY group based on its chemical composition. While potential CY chondrites exhibit significant cadmium depletion, the possibility of coincidental convergence on this matter cannot be excluded. From a mining perspective, parent bodies of CI group carbonaceous chondrites may serve as a potential source of water and, consequently, hydrogen, holding significant importance as potential fuel. Asteroid 1508 Kemi, which is a potential parent body of CI carbonaceous chondrites, may contain about 3.39·1012 Mg of water, including about 3.76·1011 Mg of hydrogen.

12

Chondryt węglisty NWA 4446

58%

Przylibski T. A. , Blutstein K. , Łuszczek K. , Gruchot J.

Przegląd Geologiczny

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2022

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tom Vol. 70, nr 7

513--526

EN

The authors carried out petrographic, mineralogical, and chemical analyses (bulk chemical composition and microanalyses of mineral chemical composition) of NWA 4446 carbonaceous chondrite. NWA 4446 chondrite is classified as CV3, S2, W2. This meteorite is a rock fragment most likely from one of the C-type asteroids orbiting the Sun in the outer part of the asteroid belt. It represents the matter formed at the earliest stages of the formation of extrasola bodies in the solar system. As a result of the research, the authors documented a wider range of variation in the chemical composition of olivine crystals (Fa: 0.67-46.57 mol%) in the matrix and chondrules, and a much narrower range of variation in the chemical com- position of pyroxene crystals (Fs: 0.90–3.35 mol%) against the data used for the classification of the meteorite. The characteristics of the chondrules, ranging in size from 0.5 to more than 1 mm, allowed concluding that they constitute about 60% of the meteorite’s vol- ume, in which they form many structural and mineral varieties PO, POP, BO, PP and RP chondrules were observed. The remaining 40% of the chondrite volume is a matrix consisting of small crystals of pyroxenes, olivines, glass, as well as opaque minerals: sulphides, FeNi alloy, native copper and gold grains, carbonaceous substance, and compact CAIs. The mineral and chemical composi- tion of CAIs shows that their dominant mineral is melilite, accompanied by diopside and spinel. The chemical composition of spinel and diopside is very similar to their total chemical formulas, while the composition of melilite shows a significant sodium deficiency. Among the opaque minerals, one phase of the FeNi dominates - awaruite (Ni 3 Fe), and sulphides are represented by troilite (FeS) and mackinawite ((Fe,Ni) 9 S 8 ). Moreover, grains of native copper with an admixture of gold and grains of native gold with an admixture of platinum, nickel and copper with a size of several μm were identified. Taking into account the admixtures contained in the above-mentioned opaque minerals (mainly Co and Cu), the parent rock of the carbonaceous chondrite NWA 4446 can be considered to have been mineralized with Fe, Ni, Co and Cu ore minerals with the content of Au and Pt. This means that, we can expect deposits of native forms of the above-mentioned metals and sulphides on the parent bodies of carbonaceous chondrites of the CV group - C-type asteroids.