Abstract
μXRF can efficiently and non-destructively aid the understanding of the chemical structure of the Murchison and Allende meteorites. In this study, was determined 15 major and minor elements (Mg, Al, Si, P, S, K, Ca, Ti, V, Cr, Mn, Fe, Ni, Fe, Zn) at meteorites carbonaceous chondrites. In addition, through the μXRF technique, it was also possible to obtain relatively precise qualitative data on where and how each of these chemical elements is related to Murchison and Allende meteorites. In this way, based on the results obtained, a brief comparative synthesis was made between the analysis of our results with some works selected from the scientific literature that use destructive analytical techniques to obtain these chemical elements. The comparative analysis demonstrates that the results were satisfactory and therefore, the use of μXRF appears to be efficient as a non-destructive analytical technique for the chemical analysis of these rare artifacts, which are meteorites
Highlights
Meteorites are excellent study materials because they are historical astrophysical artifacts that possess the chemical, physical and all geological evolution present in their materials
The qualitative determination of the chemical elements present in a both meteorites were done in a non-destructive way, that is, it did not result in the damage of the sample or in the possible loss of some future information, if it is analyzed again
The comparative analysis demonstrates that the results generated from our methodology based on the use of μXRF as an analytical technique in the Murchison and Allende meteorites was quite satisfactory
Summary
Meteorites are excellent study materials because they are historical astrophysical artifacts that possess the chemical, physical and all geological evolution present in their materials. In this way, the abundance of chemical elements present in these materials is extremely relevant for Astrobiology and Planetary Sciences because they retain unique information about the natural processes that occurred at the beginning of the Solar System. The analyses and characterization of meteorites are mostly done by destructive techniques and wet chemical methods (JAROSEWICH, 1990) Such methods require, in addition to a sample preparation, a large amount of material. The sensitivity in these terms of these techniques restricts the possibility of obtaining data, mainly due to the physical composition of the analyzed materials being modified after all
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