“三江”地区与青藏高原内部早第三纪高镁钾质岩地球化学对比:地幔源区的差异及其意义

"三江"地区和青藏高原内部广泛分布有新生代早第三纪高镁钾质岩(MgO6%,K2O/Na2O1),通常认为它们应起源于地幔源区,虽然它们均有着富钾、富集LILE和亏损HFSE的共同特征,并在形成时代上有着一致性,但青藏高原这些在不同区域的早第三纪火山岩在地球化学特征有显著的差异。"三江"地区同高原内部高镁钾质岩相比具有明显高的εNd(t)值,指示前者起源于一个相对亏损的富集地幔源区。青藏高原早第三纪高镁钾质岩可能源于与古俯冲环境相联系的富集地幔源区,但不同地区的富集物质和地幔源区矿物组成以及形成深度却是各不同。青藏高原内部高镁钾质岩的形成可能与高原腹部始新世下地壳的拆沉有关;而"三江"地区早第三纪高镁钾质岩可能与发生在50～40Ma北向俯冲的特提斯大洋板片断离有关。同时早第三纪特提斯大洋板片的北向俯冲和断离对"三江"地区在该时期的成矿物质的富集和成矿过程有着重要的贡献。     

湘黔桂地区中上二叠统硅质岩的地球化学特征及沉积背景

我国华南地区二叠系广泛发育硅质岩,但其沉积背景,如硅的来源和沉积环境,一直存在较大的争议。在对湘黔桂地区硅质岩进行大量的野外和室内岩石学研究的基础上,本文对研究区内黔桂盆地和湘桂盆地中14个不同产地的81件中上二叠统硅质岩(中二叠统33件、上二叠统48件)的主量和稀土元素进行了研究。中二叠世时期,Al2O3、TiO2、Al2O3/(Al2O3+Fe2O3)、∑REE、Ce/Ce*等整体上偏低,但具有比较一致的区域性差异:黔桂盆地相对偏低(0.09%~0.37%、0.00%~0.01%、0.22~0.47、2.47×10-6~14.59×10-6、0.23~0.69),而湘桂盆地(0.01%~5.73%、0.00%~0.23%、0.02~0.71、7.07×10-6~141.0×10-6、0.24~1.22)相对偏高。晚二叠世时期,Al2O3、TiO2、Al2O3/(Al2O3+Fe2O3)、∑REE、Ce/Ce*等整体上偏高,其中黔桂盆地分别为1.62%~10.67%、0.04%~0.65%、0.41~0.81、23.10×10-6~248.99×10-6、0.46~1.39,而湘桂盆地除来宾和柳州地区(0.00%~1.11%、0.00%~0.15%、0~0.42、0.55×10-6~36.59×10-6、0.27~0.83)偏低外,其他地区偏高(3.78%~21.37%、0.16%~0.91%、0.73~0.83、51.14×10-6~245.4×10-6、0.99~1.10),区域上呈东西两边高,中间低的分布趋势。中二叠统硅质岩自生铁W(Feauthig)百分含量整体偏高,仅少数低于50%。(La/Ce)N比值在黔桂盆地为1.61~5.04,湘桂盆地除来宾(2.63~4.90)外为0.82~1.94。而上二叠统硅质岩的W(Feauthig)除来宾、柳州和巴马地区大于70%外,其余地区的均小于50%。(La/Ce)N比值除来宾(2.42~4.50)外,整体上偏低,为0.69~2.47。研究区中上二叠统硅质岩Eu/Eu*基本没有明显的区域性差异,中二叠世时期,巴马地区一个样品为正异常(1.17),其余均为负异常,而晚二叠世时期,仅来宾和柳州地区显示了Eu/Eu*的正异常,其中柳州为1.07~1.22。结合Fe-Al-Mn、(La/Ce)N-Al2O3/(Al2O3+Fe2O3)、Fe2O3/TiO2-Al2O3/(Al2O3+Fe2O3)组合图解及岩石学研究,上述主量和稀土元素指标变化的结果表明:(1)中二叠统硅质岩的硅的来源相对复杂,黔桂盆地的硅质岩主要为热液,而湘桂盆地以生物来源为主,局部受到热液活动的影响;上二叠统硅质岩的硅的来源相对简单,主要为生物,仅巴马、来宾和柳州地区受到热液活动的影响。(2)中、晚二叠世热液活动范围和强度具有明显差异:中二叠世,研究区内热液活动较为广泛,但相对较弱;而晚二叠世热液活动较为局限却相对较强。(3)中二叠世黔桂盆地形成于远离陆源碎屑的边缘海盆环境,湘桂盆地为受到陆源碎屑影响的边缘海盆环境,而晚二叠世整个研究区的陆源碎屑输入增强,除来宾和柳州地区外,其余地区均为受陆源碎屑影响的边缘海盆环境。这一变化记录了中、晚二叠世时期研究区的构造-古地理变化信息,反映了以峨眉山玄武岩为代表的地幔柱引起的火山热液活动和区域性地壳抬升事件。     

Petrological discrimination among Precambrian dyke swarms: Eastern Kaapvaal craton (South Africa)

Age-determinations on a complex array of mafic dykes across the eastern Kaapvaal craton (Olsson et al., 2010) are complemented herein by field evidence, dyke trend analysis, and petrological characterization of 58 dyke samples. ∼2.95 Ga SE-trending, a ∼2.65 Ga E- to SE-radiating, and ∼1.90 Ga NE-trending swarms can be distinguished. Prominent Archean (∼2.95 and ∼2.65 Ga) dyke ridges contain basement xenoliths, and have a more quartz-oversaturated, andesitic and calc-alkaline character. Proterozoic (∼1.90 Ga) dykes are, on the other hand, more aeromagnetically prominent tholeiitic basalts with higher modal (Fe, Ti)-oxide contents. Multi-elemental statistics indicate that the best geochemical discrimination is found between Archean high-Sr/V and La/Yb and Proterozoic low-Sr/V and La/Yb dyke swarms. The calc-alkaline character of Archean dyke swarms is augmented by LILE-enriched spider-element patterns with steeper REE-slopes as compared to the Proterozoic swarm. Geochemical similarities are roughly consistent with the ∼2.95 and ∼2.65 Ga dykes having fed coeval lavas within the Nsuze Group and Allanridge Formation (upper Ventersdorp Supergroup), respectively. ∼1.90 Ga dykes match coeval sills on both the Zimbabwe and Kaapvaal cratons, and are presumed feeders to Soutpansberg Group lavas. This new information provided by dated feeder dyke swarms leads to a re-evaluation of petrotectonic settings, ranging from continental back-arc to radiating swarms emanating from igneous (plume?) centers.     

Bacterial calcification as a possible trigger for francolite precipitation under sulfidic conditions

Francolite (carbonate-fluor-apatite) is known to form in sediments where intense organic-matter decay occurs, but under oxic-to-suboxic conditions, because the alkalinity rise accompanying bacterial sulfate reduction (anoxic conditions) increases francolite solubility, hence preventing its supersaturation and precipitation. However, lagoonal, organic matter-rich, cryptalgal carbonates of Jurassic age located in the French Jura Mountains contain francolite that formed during early diagenesis, under anoxic-sulfidic and highly alkaline conditions. To explain this paradoxical situation, we propose the following “chain of reactions”: the presence of abundant biomass in the sediment would supply the “raw material” to the reactional system, i.e., the initial P budget, released through organic decay. The development of cryptalgal, bacterial mats at the sediment–water interface would have limited exchanges between the water column and the pore space, hampering pore water renewal and favoring the early onset of sulfate-reducing reactions. The onset of sulfate reduction would increase pore water alkalinity, potentially preventing francolite precipitation. In addition, the presence of sulfide ions would induce organic matter sulfurization, resulting in a relative pH rise. Alkalinity and pH rises would trigger the development of conditions leading to carbonate supersaturation, inducing bacterial-structure calcification. The sudden fall in alkalinity induced by early calcification would allow francolite precipitation, despite sulfidic conditions.     

Hydration state of zeolites, clays, and hydrated salts under present-day martian surface conditions: Can hydrous minerals account for Mars Odyssey observations of near-equatorial water-equivalent hydrogen?

Thermodynamic data for several clays, zeolites, and MgSO₄ salts were combined with calculated yearly mean temperatures and water-vapor pressures on the martian surface to predict mineral hydration states from low to middle latitudes. These predictions were used to evaluate whether the necessary amount and distribution of hydrous minerals were compatible with the Mars Odyssey observations of water-equivalent hydrogen (WEH). Our results indicate that zeolites like chabazite or clay minerals like Ca-montmorillonite would have to be unrealistically abundant in the martian soil (as much as 55 wt%) while Mg-sulfate hydrates at concentrations between 2 and 11 wt% could account for the WEH. However, the geographic distribution of WEH is incompatible with a uniformly distributed mineralogy in equilibrium with the annual mean P-T environment. A heterogeneous distribution of a mixture of different hydrous minerals, reflecting a heterogeneous Mars surface geology, may better explain a significant portion of the observed near-equatorial WEH.     

Stability of hydrous minerals on the martian surface

The presence of water-bearing minerals on Mars has long been discussed, but little or no data exist showing that minerals such as smectites and zeolites may be present on the surface in a hydrated state (i.e., that they could contain H₂O molecules in their interlayer or extra-framework sites, respectively). We have analyzed experimental thermodynamic and X-ray powder diffraction data for smectite and the most common terrestrial zeolite, clinoptilolite, to evaluate the state of hydration of these minerals under martian surface conditions. Thermodynamic data for clinoptilolite show that water molecules in its extra-framework sites are held very strongly, with enthalpies of dehydration for Ca-clinoptilolite up to three times greater than that for liquid water. Using these data, we calculated the Gibbs free energy of hydration of clinoptilolite and smectite as a function of temperature and pressure. The calculations demonstrate that these minerals would indeed be hydrated under the very low-P (H₂O) conditions existing on Mars, a reflection of their high affinities for H₂O. These calculations assuming the partial pressure of H₂O and the temperature range expected on Mars suggest that, if present on the surface, zeolites and Ca-smectites could also play a role in affecting the diurnal variations in martian atmospheric H₂O because their calculated water contents vary considerably over daily martian temperature ranges. The open crystal structure of clinoptilolite and existing hydration and kinetic data suggest that hydration/dehydration are not kinetically limited. Based on these calculations, it is possible that hydrated zeolites and clay minerals may explain some of the recent observations of significant amounts of hydrogen not attributable to water ice at martian mid-latitudes.     

藏北冈塘错地区OIB型和E-MORB型玄武岩组合及大地构造意义

通过对西藏羌塘中部冈塘错地区玄武岩地球化学特征研究,发现该区有OIB型和E-MORB型两类玄武岩.对两类玄武岩进行主量元素、稀土元素和微量元素地球化学图解分析及大地构造意义探讨,结合区域地质背景,认为冈塘错地区玄武岩形成于洋岛环境,可能受地幔柱岩浆活动影响,E-MORB型玄武岩的出现说明该区可能存在洋底高原.     

张八岭群火山岩地球化学特征及其构造学意义

安徽滁州张八岭地区的张八岭群分为2组。一是下部北将军组,以千枚岩和片岩为主;二是上部西冷岩组,主要为一套变质火山岩系。张八岭岩群的细碧-石英角斑岩系主要发育于西冷岩组中,具多旋回特点。细碧-石英角斑岩系以石英角斑岩为主,细碧岩次之,角斑岩类稀少。该岩系的火山岩富碱、富钠,具双峰值特征,其主量元素、微量元素和稀土元素地球化学特征表明,它形成于非造山张性环境,为裂陷槽,是与晚元古代罗迪尼亚(Rodinia)超大陆裂解有关的岩浆作用的产物。     

香格里拉扎沙地区地球化学异常及其找矿意义

扎沙地区土壤地球化学测量共圈定10个元素组合异常。Ⅰ类异常与地质构造吻合较好,应为致矿异常,可作为重要找矿标志,对缩小找矿靶区和找矿有较好的指导意义。     

江达-维西火山岩浆弧中段德钦岩体年代学、地球化学及岩石成因

本文对江达-维西火山岩浆弧德钦岩体的寄主岩石——花岗闪长岩及其镁铁质微粒包体(MME)——闪长岩进行了详细研究。二者LA-ICPMS锆石U-Pb年龄分别为254.6±1.8Ma和253.5±1.6Ma,二者形成时代一致。地球化学研究结果表明,花岗闪长岩富K₂O和Na₂O,且K₂O>Na₂O,富Al₂O₃,A/CNK平均为0.96;闪长岩富K₂O和Na₂O,但K₂O2O,富Al₂O₃和MgO,A/CNK平均为0.72;花岗闪长岩的稀土总量低于闪长岩,二者轻重稀土分馏明显,配分曲线为右倾的轻稀土富集型;二者均富集大离子亲石元素而亏损高场强元素Nb、Ta等;二者均具有相对较高的Mg^#(58.8~65.8),并具有相对较高的相容元素Cr、Ni含量(花岗闪长岩平均值分别为115×10^-6和31.6×10^-6,闪长岩平均值分别为398×10^-6和98.2×10^-6;花岗闪长岩和闪长岩¹⁷⁶Hf/¹⁷⁷Hf的平均值分别为0.282383和0.282287,二者ε_Hf(t)平均值分别为-8.3和-11.8,反映了二者属于I型花岗岩,可能为岩浆混合作用的产物。地球化学特征及Hf同位素组成一致显示岩浆来源于地壳的部分熔融,伴有不同比例的地幔物质加入,形成于弧陆碰撞-后碰撞的构造背景,暗示金沙江结合带在~255Ma已经进入了弧陆碰撞-后碰撞的地质时期。