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

100%
Blutstein K., Przylibski T. A., Łuszczek K., Gruchot J.
Acta Societatis Metheoriticae Polonorum
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2022
|
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.
2
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Ciała macierzyste meteorytów żelaznych jako złoża metali

100%
Przylibski T. A., Donhefner H., Łuszczek K.
Acta Societatis Metheoriticae Polonorum
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2012
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vol. 3
71-103
EN
Some of M type asteroids, like 016 Psyche, 022 Kalliope, 055 Pandora, 110 Lydia, 250 Bettina, 347 Pariana, 678 Fredegundis, 771 Libera, 872 Holda, are probably the source of iron meteorites. The population of these asteroids is less than 10% of all minor bodies orbiting the Sun in the asteroid belt. In the paper we analyzed the concentrations of 19 selected metals in 1730 iron meteorites according to the groups. Base on it authors found out that beside Fe and Ni the parent bodies of iron meteorites are the richest in Co, Cu, Ge, Cr, and Ga. They are also rich in As, Pt, Mo, Os, Pd, and Ir. The iron meteorites of IVB group are the richest in metals. Meteorites belonging to this group contain the highest average concentrations of Ir, Co, W, Re, Pt, Os, Pd, Rh, Ru, Mo, and Ni. Meteorites from IAB group are the richest in Ge, As, Sb and Au. The parent bodies of iron meteorites, especially from IVB and IAB groups, can be recognized as very rich polymetallic deposits. The concentrations of most of 19 analyzed metals in iron meteorites are greater than the concentrations in Earth’s crust. Only tungsten and chromium according to their strong litophile character occur in lower concentrations than in Earth’s crust. Few of the M type asteroids, those that are the source of iron meteorites, are probably the most differentiated bodies in the asteroid belt. Their chemical composition considerably differs from the composition of CI carbonaceous chondrites. Among their the most differentiated (enriched in some elements and depleted in others) and differing from CI chondrites are the parent bodies of iron meteorites belonging to IVB group. However even they are far less differentiated than Earth’s crust. This is the proof of relatively long chemical evolution of IVB group parent body comparing to parent bodies of other groups of iron meteorites and CI chondrites, but from the other hand the evolution of this body is also significantly shorter than the chemical evolution of Earth’s crust.
3
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Skład chondrytów zwyczajnych a potencjalne surowce pasa planetoid

84%
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.
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