Full-text resources of PSJD and other databases are now available in the new Library of Science.
Visit https://bibliotekanauki.pl
Preferences help
Polish version English version Language
enabled [disable] Abstract
Number of results

Results found: 1

Number of results on page
first rewind previous Page / 1 next fast forward last

Search results

help Sort By:

help Limit search:
first rewind previous Page / 1 next fast forward last
1
Publication available in full text mode
Content available

Ciała macierzyste meteorytów żelaznych jako złoża metali

100%
Przylibski T. A., Donhefner H., Łuszczek K.
Acta Societatis Metheoriticae Polonorum
|
2012
|
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.
first rewind previous Page / 1 next fast forward last
JavaScript is turned off in your web browser. Turn it on to take full advantage of this site, then refresh the page.