肇东和亳县陨石中的黑包体及其成因意义

肇东、毫县陨石中的黑包体在总体成分、形状、大小上与陨石球粒相似,但两者的内部结构以及矿物组合不同。黑包体中矿物呈密堆状,主要由细粒橄榄石以及其它硅酸盐微晶组成,不含火成玻璃等特点表明黑包体未经历过熔融,它们可能是形成球粒的毛坯。因此认为球粒的形成有三个阶段:星云凝聚形成尘粒—尘粒吸积形成黑包体—黑包体熔融形成球粒。     

肇东陨石高压加热—熔融实验研究

在30kbar压力下进行了肇东陨石的加热-熔融实验。实验结果表明。从840℃至2050℃,陨石中的金属-硫化物相经历了熔融—两相混溶的过程,最终形成一种Fe、Ni、Co、S之比不相等的多相混合物。而陨石中的硅酸盐相经历了热变质—熔融—熔融分异的过程。初熔温度为1610℃,2050℃时熔体发生分异,有富Si、Al的硅酸盐新相分离出来。以上述结果为依据,本文对类地行星早期层圈构造的形成机制进行了探讨和推论。     

Grove Mountains (GRV) 020043: Insights into acapulcoite-lodranite genesis from the most primitive member

Although acapulcoites and lodranites played a key role in understanding partial differentiation of asteroids, the lack of samples of the chondritic precursor limits our understanding of the processes that formed these meteorites. Grove Mountains (GRV) 020043 is a type 4 chondrite, with abundant, well-delineated, pyroxene-rich chondrules with an average diameter of 690 μm, microcrystalline mesostasis, polysynthetically striated low-Ca pyroxene, and slightly heterogeneous plagioclase compositions. Similarities in mineralogy, mineral composition, and oxygen isotopic composition link GRV 020043 to the acapulcoite-lodranite clan. These features include a high low-Ca pyroxene to olivine ratio, high kamacite to taenite ratio, and relatively FeO-poor mafic silicates (Fa_10.3, Fs_10.4) relative to ordinary chondrites, as well as the presence of ubiquitous metal and sulfide inclusions in low-Ca pyroxene and ƒO₂ typical of acapulcoites. GRV 020043 shows that evidence of partial melting is not an essential feature for classification within the acapulcoite-lodranite clan. GRV 020043 experienced modest thermal metamorphism similar to type 4 ordinary chondrites. GRV 020043 suggests a range of peak temperatures on the acapulcoite-lodranite parent body similar to that of ordinary chondrites, but shifted to higher temperatures, perhaps consistent with earlier accretion. The mineralogy and mineral compositions of GRV 020043, despite modest thermal metamorphism, suggests that most features of acapulcoites previously attributed to reduction were, instead, inherited from the precursor chondrite. Although partial melting was widespread on the acapulcoite-lodranite parent body, ubiquitous Fe,Ni-FeS blebs in the cores of silicates were not implanted by shock or trapped during silicate melting, but were inherited from the precursor chondrite with subsequent overgrowths during metamorphism.     

Compositions of four unusual CM or CM-related Antarctic chondrites

To identify chemical group affinities and infer the occurrence of thermal metamorphism or aqueous alteration in their histories, we quantified 43 trace elements in the CM or CM-related Antarctic carbonaceous chondrites EET 96010, LAP 02277, MET 01070, and WIS 91600. We also analyzed LAP 02206, a CV chondrite, to add to our comparison database. We present whole-rock oxygen isotope data for LAP 02206, LAP 02277, and MET 01070 to complement our trace element results. With these data, we confirm the CV classification of LAP 02206 and CM or CM-like classification for the other four chondrites in this study. On the basis of moderately volatile element content, our results show that EET 96010 experienced open-system heating, while any heating LAP 02277 and MET 01070 may have experienced was in a chemically closed-system. WIS 91600, on a trace element basis, appears to be CM-like material. Our analyses support the idea that CM material has experienced a wide variety of post-accretionary processing.     

Cratonic mantle roots, remnants of a more chondritic Archean mantle?

The Earth's continents are cored by Archean cratons underlain by seismically fast mantle roots descending to depths of 200⁺ km that appear to be both more refractory and colder than the surrounding asthenospheric mantle. Low-temperature mantle xenoliths from kimberlite pipes indicate that the shallow parts of these cratonic mantle roots are dominated by refractory harzburgites that are very old (3⁺ Ga). A fundamental mass balance problem arises, however, when attempts are made to relate Archean high-Mg lavas to a refractory restite equivalent to the refractory lithospheric mantle roots beneath Archean cratons. The majority of high-Mg Archean magmas are too low in Al and high in Si to leave behind a refractory residue with the composition of the harzburgite xenoliths that constitute the Archean mantle roots beneath continental cratons, if a Pyrolitic primitive mantle source is assumed. The problem is particularly acute for 3⁺ Ga Al-depleted komatiites and the Si-rich harzburgites of the Kaapvaal and Slave cratons, but remains for cratonic harzburgites that are not anomalously rich in orthopyroxene and many Al-undepleted komatiites. This problem would disappear if fertile Archean mantle was richer in Fe and Si, more similar in composition to chondritic meteorites than the present Pyrolitic upper mantle of the Earth. Accepting the possibility that the Earth's convecting upper mantle has become poorer in Fe and Si over geologic time not only provides a simpler way of relating Archean high-Mg lavas to the lithospheric mantle roots that underlie Archean cratons, but could lead to new models for the nature Archean magmatism and the lower mantle sources of modern hot-spot volcanism.     

胜利油区原油和沉积岩中稀土元素组成特征及其意义

文中利用稀土元素在原油运移中良好的续承性,初步探讨了在济阳坳陷内的东营凹陷和沾化凹陷原油中稀土元素的赋存特征以及它们的来源方式,并指出两凹陷不同的物源性质是造成原油稀土赋存特征差异的主要原因。     

陨石含水矿物成因评述和地球水来源的探讨

简要介绍了球粒陨石中含水矿物的种类和主要特点，根据陨石中含水矿物与无水矿物，有机质的关系，太阳星云凝聚模型中有关水蒸汽与无水矿物反应的理论，以及有关的同位素资料的综合分析，推断形成含水矿物的水化作用是太阳星云凝聚作用的一个阶段，通过不同类型球粒陨石氧同位素组成和含水矿物数量的比较，论证了太阳星云盘中发生水作用的范围，从而对地球水的来源进行了讨论。     

球粒陨石富金属Fe—Ni相的高压熔融实验与地核形成机制的探讨

选用吉林陨石富金属相,在3GPa压力、405℃～1850℃温度下,采用两种组装方式进行实验。并与先前肇东陨石全岩样的高压熔融实验进行比较。三个系列实验结果的综合对比表明,高温高压下球粒陨石中金属和硫化物经历了固相扩散、熔融和熔体聚集的过程。固相扩散使金属与硫化物彼此结合,形成了若干个小的FeNi-FeNiS二元系,使其在比Fe-Ni熔点低的温度下熔融形成Fe-Ni-S熔体。该熔体与硅酸盐熔体不相混溶,因而发生自身的合并与聚集。其合并和聚集速率与硅酸盐粘度有关。实验过程中陨石里的磷酸盐矿物可以被还原,使单质P进入金属硫化物相。这些实验结果为讨论地核的形成机理提供了依据。     

Evaluation of a curve-fitting method for diffuse reflectance spectra in the UV–Visible–NIR wavelength region

The Modified Gaussian Method (MGM) proposed by Sunshine et al. [Sunshine, J.M., Pieters, C.M., Pratt, S.F., 1990. Deconvolution of mineral absorption bands: an improved approach. Journal of Geophysical Research 95, 6955–6966.] is generally used to decompose spectra in the UV–Visible–NIR wavelength region into the characteristic absorption bands of minerals. Here, we compare the optimized results obtained using different curve-fitting methods for this spectrum. The result obtained using the Gaussian function for the absorption band shows a better fit than that obtained using the Lorentzian function. The background continuum of a quadratic polynomial for the wavenumber provides a better result than does the linear function for the wavenumber. We successfully decomposed the spectra of ordinary chondrites and eucrites into the absorption bands of olivine and pyroxene. The wavelength positions of these absorption bands are broadly consistent with the Fe contents of olivine and pyroxene. Although the present results are derived from a limited number of spectra, they are of use in terms of the decomposition of diffuse reflectance spectra.