The elemental abundances in interplanetary dust particles
The elemental abundances in interplanetary dust particles
复制标题
行星际尘埃粒子中的元素丰度
DOI：
--
复制
发表时间：
1996
期刊：
影响因子：
--
通讯作者：
E. Jessberger
中科院分区：
文献类型：
--
作者：
P. Arndt;J. Bohsung;M. Maetz;E. Jessberger
- 我们编制了一个表格，列出了89个行星际尘埃颗粒（IDP）中所有主要，次要和痕量元素的丰度，其中包括质子诱导X射线发射（PIXE），同步X射线荧光（SXRF）和二次离子质谱（西姆斯）获得的数据。第一次，国内流离失所者的微量元素丰度的可靠性进行了测试，各种交叉。我们还报告的聚类分析，我们对IDP组合物进行的结果。由于数据集的不完整性，我们只包括元素Cr，Mn，Ni，Cu和Zn，归一化为Fe和Cl球粒陨石丰度，这是在73个IDP确定。数据安排自己在四个相当不明确的组，我们讨论的CI丰度的假设，平均CI丰度是最有可能的。最大的一组（方解石），有44个成员，有许多难熔和中等难熔元素（Na，Al，Si，P，K，Sc，Ti，V，Cr，Co，Ge，Sr）的丰度接近CI。微量元素Fe亏损，Ca、S亏损较多，挥发性元素Cl、Cu、Zn、Ga、Se、Rb富集=1.7 × Cl，Br富集21 × Cl。低锌组有12个成员，除贫锌、贫钙和富铁外，与贫锌组非常相似。低Ni组有11个成员，Ni/Fe = 0.03 × CI，Ca几乎呈CI状，但其地外起源尚不成立。最后一组（6个成员）包含来源不明的非系统粒子。我们发现Fe在微米尺度上是不均匀分布的。此外，在其检测极限附近测量的元素丰度很容易被高估。所涉及的这些偏见、不完整的数据集和可能的污染过程使我们无法从元素丰度中获得关于境内流离失所者具体来源的信息。
— We compiled a table of all major, minor, and trace-element abundances in 89 interplanetary dust particles (IDPs) that includes data obtained with proton-induced x-ray emission (PIXE), synchroton x-ray fluorescence (SXRF), and secondary ion mass spectrometry (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 that 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 =1.7 × CI and Br by 21 × CI. The low-Zn group, with 12 members, is very similar to the chondritic group except for its Zn-depletion, stronger Ca-depletion and Fe-enrichment. The low-Ni group, with 11 members, has Ni/Fe = 0.03 × CI 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 Fe 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 prevent us from obtaining information on the specific origin(s) of IDPs from elemental abundances.