Search results

1

Kratery meteorytowe na Marsie

100%

Hurnik H.

Acta Societatis Metheoriticae Polonorum

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2011

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vol. 2

40-56

EN

Meteorite craters, volcanoes and deep valleys are main obiects of Mars topography. The are many tausend or millions of craters and they are very different, with diameters of only centimeters to big basins with diameters of 25oo kilometers. The age of oldest craters on Mars is about 3,9 billions year.

2

Meteoryty i kolekcjonerstwo w świetle prawa

100%

Grajewski A.

Acta Societatis Metheoriticae Polonorum

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2017

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vol. 8

52-62

EN

The ownership of meteorites is not directly regulated by the Polish law. The legislator did not sufficiently dealt with this issue, although in the case of finding a meteorite formed unregulated problem. In addition, the environment uses a large number of collectors and meteorite hunters, who can not unambiguously clarify the legal situation in which they move. In such a situation at the beginning there is a lot of questions and above all who is the owner found a meteorite, or you can without permission or a license to search for and extract meteorites, what about selling the found specimen? In order to answer the questions posed above should give you some rules that will introduce ambiguity related to this issue. This brief characterization of the issues I will show, with the vast problems we face and will answer questions.

3

NWA 14360 – Nowy meteoryt z Nigru

100%

Karwowski Ł., Szopa K.

Acta Societatis Metheoriticae Polonorum

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2022

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vol. 13

47-59

EN

The new meteorite was bought as one single stone in 2019 from a dealer in Niger by Tomasz Jakubowski. The meteorite has fusion crust. It contains chondrules of different types with dominance of barred olivine chondrules, with diameter to 1.5 mm. Px and Ol are 78.1 vol%. of the meteorite mass. Pl is up 11.8 vol%. Average fayalite content is 24.93. Metallic phases are 3.0 vol%. Troilite is up to 5.9 vol%. Spinel (Cr-spinel) is up to 0.9 vol%. Average content of the secondary Fe-rich minerals (e.g. hydroxides) is 0.4 vol%. Feldspar composition is: Ab80.2Or5.0An14.8. Mean content of Al2O3, MgO and TiO2 in chromium spinel is 6.70 wt%, 2.05 wt% and 2.02 wt%, respectively. Metal phases are kamacite and tetrataenite. The kamacite has a Ni content in the range 5.83–6.81 wt%, while the Co content is in the range 0.39 to 0.56 wt%. Tetrataenite is has Ni content from 49.68 to 50.46 wt%, and Co up to 0.05 wt%. High-Ca monoclinic pyroxene, similar to diopside, is very rare. Accessory minerals are: chlorapatite and merrylite. Base on chemistry and petrography, the meteorite is classified as ordinary chondrite (L5). The main mass, a 9190 g specimen, is in Krzysztof Socha private collection. Small fragments with the total mass 71 g are stored in Museum of Earth Sciences (catalogue no: WNoZ/Mt/110) at University of Silesia in Katowice, Poland. 39 g was used for thin-section preparation and spectroscopic investigation (Mössbauer spectroscopy).

4

Badania mikroskopowe ureilitu NWA XXX

88%

Szurgot M.

Acta Societatis Metheoriticae Polonorum

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2011

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vol. 2

138-146

EN

New NWA XXX ureilite found in 2006 was investigated by optical microscopy in reflection and in transmission. Olivines, pigeonite, metal veins and dots, and carbon phases have been revealed and their features and distribution studied. Twinning of pigeonite, reduction rims, and poikilitic inclusions of olivine in large pigeonite crystals have been identified and characterized. NWA XXX meteorite belongs to olivine-pigeonite ureilites.

5

Meteoroid i meteoryt. Powrót do podstaw i definicji

88%

Przylibski T. A.

Acta Societatis Metheoriticae Polonorum

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2023

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vol. 14

157-162

EN

As a result of the discussion of the wording contained in the latest definitions of a meteoroid and a meteorite and related terms existing in scientific sources, the author slightly modified these definitions. Modifications were made in such a way that the definitions became more unambiguous and universal, and thus could refer to meteorites of any origin on any bodies of any planetary system. Ultimately, these definitions were formulated as follows: Meteoroid: A 10 mm to 1-meter-size solid object of natural origin moving in interplanetary space or coming from space and moving through an atmosphere. Meteoroids maybe primary objects or derived by the fragmentation of larger celestial bodies, not limited to asteroids, but also including moons, planets, etc. Micrometeoroid: A meteoroid between 10 mm and 2 mm in size. Meteorite: A natural solid object larger than 10 mm in size, derived from a celestial body (or being a celestial body itself), that was transported by natural means from the body on which it formed to a region outside the dominant gravitational influence of that body, and that later collided with a natural or artificial body larger than itself (even if it is the same body from which it was launched). Weathering processes do not affect an object’s status as a meteorite as long as something recognizable remains of its original minerals or structure. An object loses its status as a meteorite if it is incorporated into a larger rock that becomes a meteorite itself. Micrometeorite: A meteorite between 10 mm and 2 mm in size. Interplanetary dust particle (IDP): A particle smaller than 10 mm in size moving in interplanetary space or coming from space and moving through an atmosphere. If such particles subsequently accrete to larger natural or artificial bodies, they are still called IDPs. The vaporised material after the meteor phase, that condenses into solid matter is called meteoric smoke. Physical phenomena (light, heat, shock, ionization) resulting from the high-speed entry of a solid object from space into an atmosphere are called a meteor. Meteors can occur on any planet or moon with a sufficiently dense and thick atmosphere. The advantage of defining the terms: meteoroid, meteorite and meteor separately and not linking these definitions to each other is the possibility of a more precise and logical definition of a meteoroid and a much broader, more universal definition of the term meteorite, not limiting it only to terrestrial conditions.

6

Batymetria jezior meteorytowych w rezerwacie „Meteoryt Morasko”

88%

Choiński A., Ptak M.

Acta Societatis Metheoriticae Polonorum

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2017

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vol. 8

23-29

EN

The paper presents results of bathymetric measurements performed on three crater lakes located in the “Meteoryt Morasko” reserve in west Poland. The maximum depth of the largest of the analysed lakes (1695 m2) was determined to amount to 2.6 m. The parameters of the lake (surface area, depth, etc.) are largely determined by a ditch dug through the crater in the north-western part of the lake, affecting the maximum water volume accumulated in the lake.

7

Historia oraz stan obecny Polish Fireball Network

88%

Wiśniewski M., Żołądek P., Olech A., Tymiński Z., Maciejewski M., Raj A., Fietkiewicz K., Gozdalski M., Gawroński M. P., Suchodolski T., Myszkiewicz M., Stolarz M., Polakowski K.

Acta Societatis Metheoriticae Polonorum

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2018

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vol. 9

177-186

EN

The Polish Fireball Network (PFN) is a project to monitor regularly the sky over Poland in order to detect bright fireballs. In 2016 the 72 PFN cameras recorded 100 389 meteor events. Using these data and the UFOOrbit software 19 087 trajectories and orbits were calculated. In the following years we are planning intensive modernization of the PFN network including installation of dozens of new digital cameras.

PL

Polish Fireball Network (PFN) to projekt polegający na regularnym monitorowaniu nieba nad Polską w celu zaobserwowania jasnych meteorów i bolidów. W 2016 roku 72 kamery PFN zarejestrowały 100 389 meteorów. Za pomocą tych danych i oprogramowania UFOOrbit obliczono 19 087 trajektorie i orbity. W kolejnych latach planujemy intensywną modernizację sieci PFN, w tym instalację kilkudziesięciu nowych kamer cyfrowych.

8

Badania ureilitu NWA XXX za pomocą analitycznej mikroskopii elektronowej

88%

Szurgot M.

Acta Societatis Metheoriticae Polonorum

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2009

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vol. 1

137-141

EN

New NWA XXX ureilite was investigated by analytical electron microscopy to determine elemental and mineral composition of the meteorite. The main minerals: olivines and clinopyroxenes have been identified and characterized. The texture, elemental and mineral composition of the meteorite are typical of olivine-pyroxene achondrites.

9

Nowy chondryt zwyczajny L6, S1, W1: Northwest Africa 11779

75%

Przylibski T. A., Łuszczek K., Kryza R.

Acta Societatis Metheoriticae Polonorum

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2019

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vol. 10

121-139

EN

Based on petrological, mineralogical and geochemical research authors classified new meteorite Northwest Africa 11779 as the ordinary chondrite L6, S1, W1. Chemical composition of olivine crystals (Fa 24.9 mol.%) and of pyroxene crystals (Fs 19.4 mol.%) proved that this meteorite belongs to L chondrites. However, bulk chemical composition of NWA 11779 is not typical for L chondrites. Nevertheless, all analyzed elements (except Mo, Sn and Nb) are in abundances reported for L chondrites, some of elements have concentration closed to average abundances for L chondrites. The content of chosen, characteristic lithophile, siderophile and chalkophile elements in NWA 11779 chondrite is in most cases in accord with its typical abundance in L chondrites. Presence of poorly defined chondrules, secondary feldspar crystals larger than 50 µm in size, absence of glass within chondrules, coarse recrystallized matrix (with olivine crystals of 0.5 mm in diameter and pyroxene crystals of 0.3 mm in diameter) as well as carbon content below 0.2 wt% proved that studied meteorite belongs to the petrologic type 6. The only difference from characteristic features of petrologic type 6 in case of NWA 11779 chondrite is presence of ca. 10% of monoclinic Ca-poor pyroxenes. Undulatory extinction by olivine and absence of other shock features in this chondrite allow to determine the shock level as S1. Weathering grade of NWA 11779 was identified as W1 based on weathering of only FeNi alloy grains. The outer part of metallic grains as well as contact zones of FeNi and FeS are changed due to weathering. Between 10 and 20% of FeNi alloy grains are oxidized to iron oxides and hydroxides. These secondary products of weathering replace outer zone of FeNi grains and fill the small cracks, creating a few thin veins.

10

Spadki meteorytów w latach 2020–2021. Okoliczności i obserwacje

75%

Morys J., Żmija M.

Acta Societatis Metheoriticae Polonorum

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2022

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vol. 13

67-106

EN

The paper presents the circumstances and data accompanying meteorite falls in recent years. The study contains descriptions of 21 falls observed in 2020 and 15 falls in 2021. These phenomena took place on all continents, except the polar regions. In conclusion, this work is a collection of several dozen stories about freshly fallen meteorites. They show many aspects connected with the observations and the hunting for new specimens.

11

Planimetrowanie ziaren FeNi jako metoda ustalenia stopnia wietrzenia W0–W4 chondrytów zwyczajnych

75%

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

Acta Societatis Metheoriticae Polonorum

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2019

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vol. 10

111-120

EN

Wlotzka scale (Wlotzka 1993) is commonly used to determine the weathering grade of ordinary chondrites. The scale is descriptive and based mostly on a subjective assessment of researcher. In this paper authors define a new, quantitative method to establish the W0–W4 weathering grade, which is based on planimetry of FeNi grains. Results of planimetry are compared with average content of FeNi metal in unweathered chondrites from the same group. Weathering grade estimated by this method are consistent with, or slightly different from the official one determined in classification, what proves the efficacy of the proposed method. Moreover, the method was applied to define weathering grade of meteoritic samples not classified so far: Pułtusk (W2), Thuathe (W2), Gao-Guenie (W2/W3), NWA 5205 (W3), NWA 4505 (W3), NWA 5296 (W2).

12

Skład chondrytów węglistych jako wyznacznik zasobności planetoid typu C w surowce metaliczne

75%

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

Acta Societatis Metheoriticae Polonorum

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2022

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vol. 13

7-26

EN

The chemical composition of carbonaceous chondrites was analysed in terms of the content of selected 24 metals, including noble metals and rare-earth metals. Based on the obtained results, the abundance of C-type asteroids in metallic raw materials was estimated and compared to the concentration of terrestrial deposits and the average content in the Earth’s crust. All the analysed elements, except rare earths, showed higher concentrations in carbonaceous chondrites than in the Earth’s crust, but most of them did not match the Earth’s deposit contents. The exception is Fe and Ni, the concentrations of which in carbonaceous chondrites significantly exceed the Earth’s deposit concentrations. The profitability of mining operations on C-type asteroids is also increased by the number of accompanying mineral commodities, mainly metals (Cr, Co, Cu, Au, Pt, Pd, Ag), and water ice. In addition, the parent bodies of carbonaceous chondrites occur relatively close to the moons of Jupiter and Saturn – potential space mission targets.

13

Nowy chondryt zwyczajny H5, S2, W1: Northwest Africa 11778

75%

Przylibski T., Łuszczek K., Kryza R., Blutstein K.

Acta Societatis Metheoriticae Polonorum

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2020

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vol. 11

77-97

EN

Based on petrological, mineralogical and geochemical analyses, the authors classified the new meteorite Northwest Africa 11778 as an ordinary chondrite H5, S2, W1. It is a single stone with mass 767.5 g and with well-preserved black fusion crust with brown shade (Fig. 1). This meteorite was found in Sahara Desert and it was purchased by Wroclaw University of Science and Technology, Faculty of Geoengineering, Mining and Geology from Moroccan dealer in Zagora in June 2013. The most characteristic component of analyzed chondrite are different types of chondrules (barred olivine – BO, porphyritic olivine – PO, granular olivine – GO, radial pyroxene – RP, porphyritic olivine-pyroxene – POP, cryptocrystalline – C) (Fig. 2), which constitute 75% of meteorite. Their size is in range 0.2–1.2 mm, with average chondrule size ca. 0.6 mm. Bigger porphyritic olivine chondrules with diameter up to 1.5 mm rarely occur. The chemical composition of olivine crystals (Fa 18 mol%) and pyroxene crystals (Fs 16.2 mol%) proves this meteorite to be an H chondrite (Tab. 1, Fig. 4–5, App. 1–2). The averaged concentration of major elements in the classified meteorite is comparable to their mean content in H chondrites (Fig. 8). The meteorite NWA 11778 contains only slightly less Mg and Al than average H chondrites (Tab. 2). Among the other analysed elements, values distinctly out of the range of typical concentrations for H chondrites are characteristic of Hg and Eu (lower concentration in the NWA 11778 meteorite) (Tab. 3, Fig. 8–9). The presence of chondrules with predominantly sharp boundaries (Fig. 2), secondary feldspar crystals with sizes of up to 50 mm, chiefly crystalline mesostasis and only secondarily – devitrified glass in chondrules, and transparent crystalline matrix (with olivine crystals up to 0.26 mm and pyroxenes up to 0.30 mm in size), as well as common occurrence of untwinned rhombic pyroxenes prove the classified meteorite to belong to petrological type 5. It is additionally confirmed by mean Ni content in troilite below 0.5 wt% (0.04 wt%) (Tab. 1, App. 4) and carbon content below 0.2 wt% (0.07 wt%) (Tab. 2). Undulatory extinction in some olivine and pyroxene crystals and the presence of irregular fractures in the NWA 11778 chondrite enables specifying its shock level as S2. The weathering grade adopted for the NWA 11778 chondrite was W1, as visible weathering changes cover only the marginal parts of FeNi alloy grains. As a result of the weathering of 10–20% of FeNi grains, iron oxides and hydroxides are formed. These secondary weathering Fe3+ compounds also fill cracks, forming veins running between chondrules within matrix (Fig. 3).

14

Spadki meteorytów w 2022 roku. Okoliczności i obserwacje

75%

Morys J., Żmija M.

Acta Societatis Metheoriticae Polonorum

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2023

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vol. 14

141-156

EN

In 2022, there were ten meteorites found worldwide after fresh falls. These are primarily ordinary chondrites, but one achondrite fall was also recorded. Meteorite falls occurred in the United States (3) and China (2) but also in Algeria, Brazil, Slovakia, India, and the Philippines. This paper shows how these meteorites were found and provides conclusions before future searches.

15

Spadki meteorytów w 2018 roku. Okoliczności i obserwacje

63%

Żmija M.

Acta Societatis Metheoriticae Polonorum

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2019

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vol. 10

199-221

EN

This scientific paper aims to systematize knowledge about the circumstances of meteorite falls in 2018. Eight of them were officially confirmed by The Meteoritical Society: Hamburg (USA), Ablaketka (Kazakhstan), Aba Pan (Nigeria), Mangui (China), Ozerki (Russia), Renchen (Germany), Gueltat Zemmour (Morocco), Komaki (Japan). Seven more have not yet been classified: Central Kalahari (Botswana), Glendale (USA), Benenitra (Madagascar), Bhakkar (Pakistan), Ghadamis (Libya), Elkouran (Morocco) and meteorite fall from the Sahara Desert. It turns out that the most numerous group of meteorite falls in 2018 were L6 chondrites. There were no iron or stony-iron falls. The author collected information from many different sources. He analyzed entries in the MetBull catalog, publications in social media and press reports in order to compare them with official data from previous years. In this way, he tries to prove that although the circumstances of each meteorite fall are different, coherent conclusions can be drawn from them, and these can help meteorite researchers, for example, in verifying eyewitness accounts.

16

Spadki meteorytów w 2017 roku. Okoliczności i obserwacje

63%

Żmija M.

Acta Societatis Metheoriticae Polonorum

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2018

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vol. 9

187-205

EN

This scientific paper is a summary of the meteorite falls in 2017: Broek in Waterland (Holland), Tres Irmaos (Brazil), Serra Pelada (Brazil) and Kheneg Ljouâd (Morocco). The study also includes a section about unconfirmed falls, such as Puya Medio (Colombia), Mukundpura (India), Crawford Bay (Canada) and Sadiya (India). The vast majority of these specimens is ordinary chondrites of the L and LL groups. Only Serra Pelada meteorite turned out to be eucrite and Mukundpura is suspected to be carbonaceous chondrite. The author collects and organizes basic information about these findings and compares the latest data with statistics from previous years. The description of the circumstances of finding meteorites are brief and maintained in the popular-scientific tone. The text also includes a set of fireballs and bolides that could end with a meteorite fall. Among them is also a bolide that was visible from Poland. The thesis resembles the criteria for dividing meteors and notes the differences in their naming. It is extended by analogies and comparisons that make possible to look at the issues from different perspectives: from the statistical, through the media, to the historical one.

17

Spadki meteorytów w 2019 roku. Okoliczności i obserwacje

63%

Żmija M.

Acta Societatis Metheoriticae Polonorum

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2020

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vol. 11

141-157

EN

In 2019 two meteorite showers occurred on Earth, which ended with the fall of hundreds of fragments in Cuba and Costa Rica. Apart from them, meteorites with a total weight of probably less than 10 kg landed in Algeria, Morocco, Iran, India, and Germany. This work is another summary of the year in terms of meteorite falls. It includes information on the circumstances of these phenomena and their scientific consequences. The author collected information from many sources, especially the media and meteorite hunters, to describe in a brief form how the meteorites fell last year. The purpose of his work is to gather basic and proven knowledge, which can serve as an inspiration to further explore the history of meteorites, own meteorite hunting, and draw the attention of researchers to interesting falls in distant regions of the world.

18

Opis okoliczności i miejsca spadku meteorytu we wsi Sołtmany pod Giżyckiem oraz wstępne wyniki badań

63%

Woźniak B., Woźniak M.

Acta Societatis Metheoriticae Polonorum

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2012

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vol. 3

140-152

EN

A description of an ordinary chondrite L6 type fall in Soltmany Village. A report from a fall spot and initial results of examination carried by polish scientists team. An examination of elementary and mineral abundance and magnetic features. History of meteorite fragments.

19

Skład chondrytów zwyczajnych a potencjalne surowce pasa planetoid

63%

Łuszczek K., Przylibski T. A.

Acta Societatis Metheoriticae Polonorum

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2011

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vol. 2

92-111

EN

In this article the authors present a simple method of determining the content of selected metal raw materials (Fe, Ni, Co) on the parent bodies of ordinary chondrites. Thanks to the use of planimeter for measuring, under microscope, polished slices of meteorites, it is possible to estimate quite accurately the proportion of these metals in the parent bodies of meteorites, i.e. on asteroids. When it comes to analysing a large number of polished slices, these results will be most likely comparable to much more expensive results of chemical tests conducted on meteorites. Based on the analysis of 16 thin polished sections and polished slices of 11 ordinary chondrites, the authors found out that the highest content of Fe, Ni and Co ore minerals, reaching 10,06% of the total volume, can be found in ordinary chondrites from group H. For ordinary chondrites from groups L and LL, it makes 3,86% and 3,93% of the volume respectively. Employing the results of chemical analyses available in literature sources, the authors also estimated the size of Fe, Ni and Co resources for several selected asteroids. These bodies contain higher concentrations of iron, nickel and cobalt than terrestrial deposits (those found in the earth’s crust). The total content of Fe on parent bodies of even the most deficient in metals group LL of ordinary chondrites is about twice as high as that in the earth’s crust. Cobalt occurs on parent asteroids of ordinary chondrites in concentrations 15–24 times as high as those in the earth’s crust, and the concentrations of Ni are 100–180 times as high as those in the earth’s crust. The contents of these metals on parent asteroids of ordinary chondrites are also several times as high as those in currently extracted deposits in the earth’s crust. Taking into account the mean annual terrestrial production of these metals, the authors have estimated that a parent asteroid of ordinary chondrites with the size between 433 Eros and 6 Hebe could satisfy our need for Fe, Ni and Co for the nearest several million to dozens of billion years. Considering the fact that asteroid belt contains plenty of such objects, and as many asteroids built chiefly of Fe-Ni alloy, one should regard this section of the Solar System as a practically inexhaustible source of metal raw materials. The prospect of their exploitation is probably much nearer than we can currently imagine.

20

Chondryt Sołtmany

39%

Przylibski T. A.

Acta Societatis Metheoriticae Polonorum

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2016

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vol. 7

93-122

EN

The Sołtmany hammer meteorite is classified as an ordinary chondrite type L6, W0, S2. At present it is the most thoroughly and comprehensively examined Polish meteorite. A comprehensive petrological, mineralogical and geochemical analysis alongside the investigation of its physical and particularly thermophysical properties, and, most of all, analyses of cosmogenic radionuclides and noble gases isotopes content, as well as the use of a troilite thermometer has made it possible to draw interesting conclusions concerning the genesis and evolution of the parent body and the history of the parent meteoroid and, finally, the Sołtmany meteorite. The present report attempts at summing up the results of studies conducted at several European research centres in the last four years. The age of the the Sołtmany chondrite parent rock has been defined at 4.137 billion years. It was formed at a temperature of up to 440–450 K (about 170°C), probably at a depth of up to 3 to 7 km under the surface of the parent body, i.e. at a pressure of the order of 1–2.4 kbar. Such a low temperature during the accretion, diagenesis and metamorphism of the parent body may point to its complicated development, which may be in part due to collisions of partially melted planetesimals. Like with other type L ordinary chondrites, one can infer that the parent body could have been destroyed about 467 million years ago, at the time of a catastrophic collision which led to the formation of Gefion family of planetoids. Perhaps one of the bodies in this family was involved in another collision about 29.2 million years ago, which resulted in ejecting the parent meteoroid of the Sołtmany chondrite onto the Earth collision trajectory. Before entering the Earth’s atmosphere, this meteoroid had the mass of about 36 kg and the diameter of ca 13.5 cm. During its flight through the atmosphere, it rotated and somersaulted, which resulted in the formation of an uniform thin (0.5–0.7 mm) fusion crust, whose temperature reached 1000°C. In the last phase, the Sołtmany meteorite fell almost vertically and its mass was a mere 3% of the mass of the parent meteoroid – 1.066 kg. It hit the roof and then the concrete stairs of a farm building, which caused it to break into two bigger and many small pieces. It was found a few minutes after the fall, which occurred at 6:03 a.m. (CEST, UTC+2:00) on 30 April 2011, by Wydmińskie Lake in northern Poland (54°00,53’N, 22°00,30’E). The Sołtmany chondrite is one of just 14 meteorites in which the activity concentration of the cosmogenic 52Mn has been determined, and one of the few ordinary chondrites where the concentration of organic matter has been defined. As a result, it was found out that unlike in carbonaceous CI chondrites, the composition of organic particles is dominated by less complex compounds (CHO and CHOS) than CHNO and CHNOS compounds. This may indicate the decomposition of more complex organic compounds into particles with simple structures during magmatic and metamorphic processes related to formation of type L ordinary chondrites.

Refine search results

Kratery meteorytowe na Marsie

Meteoryty i kolekcjonerstwo w świetle prawa

NWA 14360 – Nowy meteoryt z Nigru

Badania mikroskopowe ureilitu NWA XXX

Meteoroid i meteoryt. Powrót do podstaw i definicji

Batymetria jezior meteorytowych w rezerwacie „Meteoryt Morasko”

Historia oraz stan obecny Polish Fireball Network

Badania ureilitu NWA XXX za pomocą analitycznej mikroskopii elektronowej

Nowy chondryt zwyczajny L6, S1, W1: Northwest Africa 11779

Spadki meteorytów w latach 2020–2021. Okoliczności i obserwacje

Planimetrowanie ziaren FeNi jako metoda ustalenia stopnia wietrzenia W0–W4 chondrytów zwyczajnych

Skład chondrytów węglistych jako wyznacznik zasobności planetoid typu C w surowce metaliczne

Nowy chondryt zwyczajny H5, S2, W1: Northwest Africa 11778

Spadki meteorytów w 2022 roku. Okoliczności i obserwacje

Spadki meteorytów w 2018 roku. Okoliczności i obserwacje

Spadki meteorytów w 2017 roku. Okoliczności i obserwacje

Spadki meteorytów w 2019 roku. Okoliczności i obserwacje

Opis okoliczności i miejsca spadku meteorytu we wsi Sołtmany pod Giżyckiem oraz wstępne wyniki badań

Skład chondrytów zwyczajnych a potencjalne surowce pasa planetoid

Chondryt Sołtmany