The elemental abundances in interplanetary dust particles

Details The elemental abundances in interplanetary dust particles The elemental abundances in interplanetary dust particles

Oct 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996m%26ps...31..817a&link_type=abstract

Meteoritics, vol. 31, pages 817-833.

Computer Science

19

Scientific paper

We compiled a table of all major, minor, and trace element abundances in 89 IDPs that includes data obtained with PIXE, SXRF, and SIMS. For the first time the reliability of the trace element abundances in IDPs is tested by various crosschecks. We also report on the results of cluster analyses that we performed on IDP compositions. Because of the incompleteness of the data set we included only the elements Cr, Mn, Ni, Cu, and Zn, normalized to Fe and CI chondrite abundances, that are determined in 73 IDPs. The data arrange themselves in four rather poorly defined groups which we discuss in relation to CI chondrites following the assumption that on the average CI abundances are most probable. The largest group (chondritic) with 44 members has close to CI abundances for many refractory and moderately refractory elements (Na, Al, Si, P, K, Sc, Ti, V, Cr, Co, Ge, Sr). It is slightly depleted in Fe and more in Ca and S, while the volatile elements (Cl, Cu, Zn, Ga, Se, Rb) are enriched by ;1.74CI and Br by 214CI. The low-Zn group with 12 members is very similar to the chondritic group except its Zn-depletion, stronger Ca- depletion and Fe-enrichment. The low-Ni group with 11 members has Ni/Fe=0.034CI and almost CI-like Ca but its extraterrestrial origin is not established. The last group (6 members) contains non-systematic particles of unknown origin. We found that iron is inhomogeneously distributed on a micron scale. Furthermore the abundances of elements that are measured near their limits of detection are easily overestimated. These biases involved, the incomplete data set, and possible contaminating processes until now prevent to obtain information on the specific origin(s) of IDPs from elemental abundances.

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