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2012 | 3 | 71-103
Article title

Ciała macierzyste meteorytów żelaznych jako złoża metali

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Title variants
EN
Parent bodies of iron meteorites as metal ores deposits
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PL
Abstracts
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.
Publisher

Year
Volume
3
Pages
71-103
Physical description
Contributors
  • Politechnika Wrocławska, Wydział Geoinżynierii, Górnictwa i Geologii, Instytut Górnictwa, Zakład Geologii i Wód Mineralnych, Tadeusz.Przylibski@pwr.wroc.pl
  • Politechnika Wrocławska, Wydział Geoinżynierii, Górnictwa i Geologii, Instytut Górnictwa, Zakład Geologii i Wód Mineralnych
  • Politechnika Wrocławska, Wydział Geoinżynierii, Górnictwa i Geologii, Instytut Górnictwa, Zakład Geologii i Wód Mineralnych
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Document Type
article
Publication order reference
Identifiers
YADDA identifier
bwmeta1.element.psjd-c507cbec-5116-4aba-a9fd-4b7f5f927e8a
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