Exsolutions of Diopside and Magnetite in Olivine from Mantle Dunite, Luobusa Ophiolite, Tibet, China

The exsolutious of diopside and magnetite occur as intergrowth and orient within olivine from the mantle dunite, Luobusa ophiolite, Tibet. The dunite is very fresh with a mineral assemblage of olivine （〉95%） ＋ chromite （1%-4%） ＋ diopside （〈1%）. Two types of olivine are found in thin sections： one （Fo = 94） is coarse-grained, elongated with development of kink bands, wavy extinction and irregular margins; and the other （Fo = 96） is fine-grained and poly-angied. Some of the olivine grains contain minor Ca, Cr and Ni. Besides the exsolutions in olivine, three micron-size inclusions are also discovered. Analyzed through energy dispersive system （EDS） with unitary analytical method, the average compositions of the inclusions are： Na20, 3.12%-3.84%; MgO, 19.51%-23.79%; Al2O3, 9.33%-11.31%; SiO2, 44.89%-46.29%; CaO, 11.46%-12.90%; Cr2O3, 0.74%-2.29%; FeO, 4.26%- 5.27%, which is quite similar to those of amphibole. Diopside is anhedral f＇dling between olivines, or as micro-inclusions oriented in olivines. Chromite appears euhedral distributed between olivines, sometimes with apparent compositional zone. From core to rim of the chromite, Fe content increases and Cr decreases; and A! and Mg drop greatly on the rim. There is always incomplete magnetite zone around the chromite. Compared with the nodular chromite in the same section, the euhedral chromite has higher Fe3O4 and lower MgCr2O4 and MgAI2O4 end member contents, which means it formed under higher oxygen fugacity environment. With a geothermometer estimation, the equilibrium crystalline temperature is 820℃-960℃ for olivine and nodular chromite, 630℃-770℃ for olivine and euhedral chromite, and 350℃-550℃ for olivine and exsoluted magnetite, showing that the exsolutions occurred late at low temperature. Thus we propose that previously depleted mantle harzburgite reacted with the melt containing Na, Al and Ca, and produced an olivine solid solution added with Na^＋, Al^3＋, Ca^2＋, Fe^3＋, Cr^3＋. With temperature d     

江南造山带西段新元古代超基性岩体年代学和岩石地球化学研究及其对源区的约束

本文研究对象为江南造山带西段湘西通道地区长界橄榄辉石岩。长界橄榄辉石岩锆石LA ICP-MS U-Pb加权平均年龄为701±11 Ma。长界橄榄辉石岩主要由单斜辉石、橄榄石和少量斜长石以及少量钛铁氧化物组成,指示在岩浆形成过程中单斜辉石、橄榄石和少量斜长石为主要分离结晶相。全岩具有低SiO_2(44.01%~47.72%)、Al_2O_3(6.77%~9.10%)、TiO_2(0.49%~0.75%)和全碱(Na_2O+K_2O=0.07%~2.04%)含量,而高MgO(23.97%~30.70%)含量的特征,岩石属于亚碱性拉斑玄武岩系列。长界橄榄辉石岩稀土元素总量(∑REE)较低,为25.7×10-6~55.6×10~(-6),全岩稀土和微量元素标准化图解与洋岛玄武岩(OIB)相似,具有富集轻稀土元素[(La/Yb)N为3.36~6.48]和富集大离子亲石元素(LILE)的特点,同时还显示出"弧岩浆"的地球化学性质,明显的Nb-Ta负异常,较高的Th/Nb值(0.52~0.81)和较低的Nb/La值(0.25~0.44)以及低Nb(1.11×10~(-6)~3.91×10~(-6))的特征。长界橄榄辉石岩具有高初始(87Sr/86Sr)i值(0.707 206~0.708 561)和正的εNd(t)值(0.25~0.41)。微量元素模拟结果表明,长界橄榄辉石岩起源于尖晶石相,其源区为受来自俯冲消减板片脱水或熔融形成的流体或熔体的交代的软流圈地幔,是软流圈地幔上涌并发生低度部分熔融的产物(4%~7%)。结合区域地质特征,推测长界橄榄辉石岩的形成可能与700 Ma时期江南造山带西段裂谷作用导致软流圈物质上涌并发生熔融有关。     

橄榄石原位高温拉曼光谱研究

利用微型电阻丝加热装置产生高温, 采用镍铬热电偶探测样品的温度, 在273～1 113 K温度范围,对橄榄石晶体进行了原位高温拉曼光谱研究。拉曼光谱数据显示：Si-O伸缩振动模高于800 cm^-1,Si-O弯曲振动模为400～700 cm^-1,SiO₄四面体旋转振动模和金属-氧的平移振动模低于400 cm^-1;得到了橄榄石拉曼振动频率随温度的变化关系,首次发现了橄榄石常温频率为541 cm^-1的Si-O反对称弯曲振动的A_g模,比其它的振动频率有较弱的温度效应。     

Distribution of Olivine and Pyroxene Derived from Clementine Data in Crater Copernicus

In order to derive the distribution of olivine and pyroxene in Crater Copernicus,we compute two band ratios(950/750 and 2 000/1 500 nm) ,percent content of elements(Al%,Ca%,Mg%,FeO%) and maturity(Is/FeO) based on Clementine UVVIS and NIR image data.The central peaks of Copernicus,which are known to be olivine-rich or pyroxene-rich,are chosen as ground truth and ROIs used to derive the distribution of olivine and pyroxene with a decision tree and spectral angle mapper(SAM) .Additionally,we compared previous ...     

Discovery Of Mg-Rich Pyroxenes In Comet C/1995 O1 (Hale-Bopp): Pristine Grains Revealed At Perihelion

The NASA Ames HIFOGS spectrometer observed comet C/1995 O1 (Hale-Bopp) at epochs including 96 Oct 7–14 UT (2.8 AU), 97 Feb 14–15 UT (1.2 AU), 97 Apr 11 UT (0.93 AU), and 97 Jun 22, 25 UT (1.7 AU). The HIFOGS 7.5–13.5 μm spectrophotometry (R = 360 - 180) of the silicate feature at 2.8 AU is identical in shape to the ISO SWS spectra of comet Hale-Bopp (Crovisier et al., 1997); the strong 11.2 μm peak in the structured silicate feature is identified as olivine. Upon close passage to the sun, the HIFOGS spectra at 1.2 AU and 0.93 AU reveals strong peaks at 9.3 μm and 10.0 μm. The post-perihelion 10 μm silicate feature at 1.7 AU is weaker but has nearly the same shape as the pre-perihelion spectra at 1.2 AU, reverting to its pre-perihelion shape: there is no change in the dust chemistry by close passage to the sun. The appearance of the strong peaks at 9.3 μm and 10.0 μm at r_h ≲ 1.7 AU is attributed to the rise in the contribution of pryoxenes (clino-pyroxene and orthopyroxene crystals) to the shape of the feature, and leads to the hypothesis that the pyroxenes are significantly cooler than the olivines. The pyroxenes are radiating on the Wien side of the blackbody at 2.8 AU and transition to the Rayleigh-Jeans tail of the blackbody upon closer approach to the Sun. Composite fits to the observed 10 μm silicate features using IDPs and laboratory minerals shows that a good empirical fit to the spectra is obtained when the pryoxenes are about 150 K cooler than the olivines. The pyroxenes, because they are cooler and contribute signficantly at perihelion, are more abundant than the olivines. The perihelion temperature of the pyroxenes implies that the pyroxenes are more Mg-rich than the other minerals including the olivines, amorphous olivines, and amorphous pyroxenes. The PUMA-1 flyby measurements of comet P/Halley also indicated an overabundance of Mg-rich pryoxenes compared to olivines. Comet Hale-Bopp's pyroxenes are similar to pyroxere IDPs from the ’Spray‘ class, known for their D-richness and their unaltered morphologies: Hale-Bopp's Mg-rich pyroxenes may be pristine relic ISM grains. This revised version was published online in July 2006 with corrections to the Cover Date.     

不同粒径的月球橄榄石二向性反射特征研究

研究月表矿物组成和分布,对于探测月表地质构造以及月球的起源和演化具有重要的意义。因此,物质成分探测一直是月球研究的重点课题之一。尽管人类已经能够从月球采集样品进行实验室分析,但遥感技术仍然是研究月球的主要手段。文中主要目的是模拟不同粒径下橄榄石的二向性反射特征。为此,首先提出模拟不同粒径下反射特征的方法,然后利用Hapke模型和Mie散射理论对不同粒径下富铁和富镁橄榄石的二向性反射特征进行了模拟。模拟结果显示,富镁橄榄石的二向性反射率较富铁橄榄石的反射率高。最后,分析了反射率差值和等效粒径的相关性。该结论为选择探月传感器的波段组合、识别橄榄石镁铁含量提供了理论依据,也为应用遥感数据的橄榄石的判别奠定了基础。     

Major Element Chemical Heterogeneity in Geo2 Olivine Microbeam Reference Material: A Spatial Approach to Quantifying Heterogeneity in Primary Reference Materials

A 270 spot‐analysis study was conducted across a large (ca. 1200 μm × 1200 μm) chip of Geo2 olivine from a commercially available GEO Mk2 block (P and H Developments 2016 , Standards for EPMA), which revealed an 8.7% relative range in FeO abundance. Interleaved and overlapping grids of different resolutions were measured sequentially to prove spatial patterns are not due to drift or other external sources of error. Results were mapped and interpolated using commercially available geographical information system software, such that composition could be predicted according to location with high accuracy. The simple, systematic zonation pattern observed demonstrates that useful‐sized regions of acceptable homogeneity do exist for some elements. This knowledge allows a user to target individual regions of a characterised chip for use as distinct measurement standards. As analysis times decrease and data sets grow, this approach may maximise laboratory efficiency by characterising large chips and extending time between conventional block repolish and coating, particularly in those cases where the avoidance of prior beam damage is a key concern.     

蛇绿岩型铬铁矿床包壳纯橄榄岩中的流体过程印记:来自西藏雅鲁藏布江缝合带罗布莎和泽当岩体的地质学、岩石学和橄榄石晶体化学证据

岩浆型矿床一般认为是岩浆分异的产物,因为这类矿床通常缺乏强烈的近矿围岩蚀变。蛇绿岩中的豆荚状铬铁矿被认为是一种典型的岩浆型矿床,流行的成因模型包括岩浆通道模型和熔体-岩石反应模型。深部晶体群的大量发现,表明铬铁矿成矿系统不是一种理想系统,而是至少由两类子系统组成的复杂性动力系统。因此,流行模型不再适用,必须构建能够整合新证据的成因模型。这类矿床的典型地质特征是具有从方辉橄榄岩围岩经包壳纯橄榄岩到铬铁矿石的分带,且包壳纯橄榄岩与铬铁矿之间为渐变接触关系,包壳纯橄榄岩与方辉橄榄岩之间既可以为渐变接触关系,也可以为截然接触关系或侵入接触关系。因此,阐明纯橄榄岩的成因是理解豆荚状铬铁矿形成机制的关键。西藏雅鲁藏布江缝合带中罗布莎和泽当两个代表性超镁铁质杂岩体的新观察揭示:(1)包壳纯橄榄岩的出露宽度变化于厘米级到百米级,但岩石具有均匀的细粒结构,流行模型难以解释;(2)包壳纯橄榄岩可以划分为至少两种构造类型:块状纯橄榄岩和片理化纯橄榄岩,暗示了纯橄榄岩形成过程的多阶段特点;(3)包壳纯橄榄岩主要由变晶橄榄石组成,仅含有少量由熔体或流体析出的橄榄石晶体;(4)与方辉橄榄岩相比,包壳纯橄榄岩中的橄榄石具有高MgO、Cr2O3、CaO和低MnO、Al2O3的特点,展示了矛盾的晶体化学特征;(5)邻近铬铁矿体的纯橄榄岩中常见反豆状结构,类似于多相稀释流体流体制中紊流产生的中尺度结构。上述看似矛盾的证据表明包壳纯橄榄岩的形成过程有大量深部流体的参与,因而流体过程可以作为构建一个新的整合模型的基础。据此,文中提出一个熔体-流体流模型,其基本机制是溶解-沉淀反应Opx+Fluid→Ol±Sp±Cpx±Pl±SiO2(fluid),而基本前提则是深部还原流体的持续供给和熔体-流体流的快速上升。此外,文中还表明,依据火成岩地质学、岩石学和名义无水矿物晶体化学证据也可以再造岩浆系统的流体过程。     

吉林省大石河橄榄石矿床的产出特征

吉林省大石河玄武岩规模小，并受敦－密大断裂控制。玄武岩中构成宝石的橄榄石产于二辉橄榄岩包体中和少量的捕虏晶中。矿床为碱性玄武岩，以位于大断裂次级构造上为特征。     

Intensity and direction of lattice-preferred orientation of olivine: are electrical and seismic anisotropies of the Australian mantle reconcilable?

It has been hypothesised that seismic and electrical anisotropy at the base of the lithosphere are caused by strain-induced lattice-preferred orientation (LPO) of olivine [100] axes parallel to present-day plate motion. This would imply that seismic and electrical anisotropy observations can provide geodynamicists with fundamental information for characterising mantle flow. The qualitative agreement between the fast direction of SV-waves and direction of maximum electrical conductance modelled deeper than 150 km below the North Central craton of Australia appear to support a common alignment mechanism, and the observed, anisotropic electrical conductances can be generated by hydrogen diffusivity in a water-poor (<1000 ppm H/Si) olivine mantle. A quantitative test is proposed for the hypothesis that electrical anisotropy is generated by anisotropic hydrogen diffusion rates (D) in olivine. Electrical anisotropy factors are computed using random resistor network models assuming that D[100]≈20×D[010]≈40×D[001]. Electrical and seismic anisotropies calculated from olivine LPO angular distribution functions modelled for a range of shear strains under a simple shear deformation demonstrate that the intensity of olivine [100] alignments (and associated shear strains) that would be required to explain the electrical anisotropy in the mantle below central Australia are significantly greater than predicted by Rayleigh wave anisotropies. The poor agreement between the observed electrical anisotropies and the electrical anisotropies that would be predicted from the Rayleigh wave anisotropies indicates that either (i) electrical anisotropy in the upper mantle below central Australia is not generated by hydrogen diffusivity alone or (ii) the seismic anisotropy is underestimated. The orientation of the olivine [100] axes maxima is inferred to be ∼30° rotated relative to the direction of present-day absolute plate motion (APM) that is determined relative to the hotspot reference frame (HS2-NUVEL1). Both the APM direction that is determined relative to a reference frame defined by requiring no-net rotation of the lithosphere (NNR-NUVEL1) and GPS-derived plate motion vectors fit the geophysical observations of upper mantle anisotropy better. This may support the contention that hotspots are not stationary relative to the deep mantle.