麦哲伦海山富钴结壳的稀有气体丰度及He、Ar同位素组成

使用MM5400质谱计对麦哲伦海山富钴结壳和结壳基岩进行稀有气体同位素分析,以此示踪结壳形成期间的海洋环境。富钴结壳的He、Ne、Ar、Kr、Xe稀有气体同位素丰度模式与ASW(air-saturated water,饱和空气的海水)的变化趋势一致,说明结壳是在与海水交换平衡的流体环境中形成的。结壳的分馏因子F_3比饱和空气的海水的F_3高2～3个数量级,表明其相对于海水而言是富集~3He的。其相对于空气亏损~3He、富集Kr和Xe的模式与高度富集~3He、亏损Kr和Xe的星际尘粒的模式完全不同,暗示地球外物质并不是支配富钴结壳稀有气体同位素丰度模式的主要因素。结壳中高的R值甚至超过上地幔代表MORB(大洋中脊玄武岩)的典型值8R_a(R_a为地球大气中~3He/~4He比值,R为样品中~3He/~4He比值),揭示了热点型地幔热液对西太平洋海洋环境的局部贡献。圈层结壳的各结壳层之间的R值差异明显,各结壳层之间的尺值的变化趋势是"较高→最高→较高",结壳中层具有高达15.60R_a的R值,明显有深部地幔流体的加入,这进一步表明滋养结壳生长的热液环境本质上是源于地幔柱型的热点热液。玄武质基岩具有较低的R值,说明该类基岩在形成时严重混染有地壳物质,也说明结壳的物源并非来自玄武质基岩。结壳的~(40)Ar/~(36)Ar比值接近于饱和空气的海水值,也表明结壳的成矿流体与周围海水发生了充分的交换。     

中太平洋富钴结壳不同壳层He,Ar同位素组成

对中太平洋MH海山富钴结壳不同壳层样品的稀有气体同位素丰度与组成测定结果表明:富钴结壳中He同位素组成类似于深海沉积物,主要来源于宇宙尘,其3He含量由老到新呈现基本稳定的特征,但在8Ma时3He含量明显增加,是其他样品的4～5倍,与深海沉积物中3 He含量在8Ma达到最大值相吻合.在未磷酸盐化壳层中,D4、D5、D7...     

太平洋海山富钴结壳铂族元素（PGE）和Os同位素地球化学及其成因意义

本文分析了中西太平洋海山富钴结壳及其各主要层圈(外层、疏松层、亮煤层)和玄武岩基岩的铂族元素(PGE)和Au 含量以及 Os 同位素组成,发现富钴结壳中 PGE 和 Au 含量均较高,且变化很大,∑PGE 为(70.09～629.26)×10~(-9),平均289.48×10~(-9),Au 为(0.60～26900)×10~(-9).具三层结构的富钴结壳中,疏松层(∑PGE=(339.37～545.82)×10~(-9))和亮煤层(∑PGE=(280.09～629.26)×10~(-9))的∑PGE 明显高于外层((70.09～133.27)×10~(-9).单层结壳的∑PGE 为(83.94～479.75)×10~(-9),Au 含量普遍高于具三层结构者.结壳的∑PGE 和 Au 含量远高于太平洋多金属结核(分别为(101.57～155.83)×10~(-9)和(1～4)×10~(-9)。沉积深度和海水氧逸度的不同是导致结壳和结核中 PGE 含量明显差异的主导因素。富钴结壳∑PGE 和 Pt 与 Mn(%)之间呈明显的正相关关系,而与 Fe(%)具负相关性,与多金属结核正好相反,显示结壳中的 PGE主要赋存在水羟锰矿(δ-MnO_2)等锰矿物相中,与针铁矿(FeOOH·nH_2O)等铁矿物相关系不大,而结核中的 PGE 主要赋存在铁矿物相中。PGE 球粒陨石标准化曲线和各项参数显示富钴结壳的 PGE 和 Au 主要来自海底玄武岩的蚀变释放,部分来自铁陨石微粒等地外物质,而与海底热水活动无关。计算显示西太平洋结壳距今42.5Ma 左右开始生长,生长过程中分别在8.0Ma 和21.8Ma 处出现间断,相应形成外层、疏松层和亮煤层,其各自沉积速率为2.64mm/Ma,1.45mm/Ma 和1.06mm/Ma,相应海水的~(187)Os/~(188)Os 分别为0.948～0.953,0.599～0.673和0.425～0.536,显示外层含有较多的大陆风化尘,而疏松层和亮煤层的沉积物主要来自海底洋壳蚀变和陨石碎屑或宇宙尘等地外物质。     

西太平洋海山玄武岩的岩石学特征及与上覆富钴结壳的关系

通过对西太平洋海山玄武岩和玄武质火山角砾岩的岩石学特征及其气孔充填物成分变化的研究,讨论了海山玄武岩与上覆富钴结壳的关系。富钴结壳的基岩火山岩主要为碱性玄武岩和玄武质火山角砾岩。碱性玄武岩中气孔充填物为S型和C型,S型和C型气孔充填物不共存在同一个气孔中。S型气孔充填物的物质成分富Si、Fe、K、Mg、Al,Co含量一般为0.17%~0.46%,其成分与碱性玄武岩的组成类似,其物质来源可能与碱性玄武岩有关。C型气孔充填物为O、Ca、C及少量Si、Al、Mg、Fe、K等元素,C型气孔充填物可能与海水中物质的沉积有关。由Si、Al、Fe、Mg、K等元素变化曲线反映出的S型气孔充填物沉积过程与富钴结壳早期的沉积过程具有相似的趋势,说明富钴结壳早期沉积物的物质来源可能与碱性玄武岩有关,富钴结壳物质来源可能是碱性玄武岩和海水共同作用的结果。     

相对相容性:富钴结壳微量元素富集规律研究的新指标

产出于海山表面的富钴结壳是水成成因铁锰氧化物、生物成因组分、碎屑组分等组成的复杂混合物~([1,2]).富钴结壳中金属的最终来源有河流和风输入的大陆物质、海底热液活动输入物质、海底玄武岩的风化产物,海底沉积物中释放的金属元素,以及地外物质~([2]),这些金属部分淋滤进入海水,在由海水进入水成成因铁锰氧化物,部分则以生物成因组分、碎屑组分进入结壳.     

深海沉积物中的碲异常

碲在地球上是一种稀有分散元素,碲在地壳中的丰度很低,仅为1.0ng/g;但碲在富钴结壳、海底多金属结核、深海沉积物和陨石中的丰度异常高。为了查明深海沉积物中碲异常的原因,我们对比分析了深海沉积物中磁性部分与全岩的碲含量和氦同位素组成。结果显示磁性部分的He含量和3He/4He比值及Te含量较全岩的值明显偏高;3He含量与Te含量同步变化;在3He-Te关系图上,二者具明显的正相关关系。首次提出深海沉积物中的碲异常与氦同位素异常一样可能是由宇宙尘注入引起的;海底多金属结核和富钴结壳中的碲异常可能也与宇宙尘有关。深海沉积物中的碲异…     

大洋富钴结壳资源调查与研究进展

富钴结壳是继多金属结核资源之后被发现的又一深海沉积固体矿产资源,在太平洋、大西洋和印度洋的海底均有分布。据估算,全球三大洋海山富钴结壳干结壳资源量为(1081.1661~2162.3322)×108t。世界各国对富钴结壳的调查始于20世纪80年代初,截至目前,已有日本、中国、俄罗斯和巴西等4个国家与国际海底管理局签订了富钴结壳勘探合同,而韩国的矿区申请也于2016年获得核准。富钴结壳按形态可分为板状结壳,砾状结壳和钴结核3种类型。富钴结壳内部结构构造在宏观上通常表现为三层构造,即底部亮煤层、中部疏松层和顶部较致密层;在微观下主要表现为柱状构造、叠层构造、斑块状构造、纹层状构造等多种类型。富钴结壳的矿物成分主要为自生的铁锰矿物,包括水羟锰矿、钡镁锰矿、羟铁矿、四方纤铁矿、六方纤铁矿、针铁矿等。富钴结壳富含Mn、Fe、Co、Ni、Cu、Pb、Zn等金属元素以及稀土元素和铂族元素,其中Co含量尤为显著。三大洋中,以太平洋富钴结壳的Co平均含量最高。富钴结壳的生长过程极其缓慢,平均仅几毫米每百万年。研究表明,西太平洋富钴结壳最早于始新世-早中新世开始生长。目前通常认为富钴结壳为水成成因,即Co、Fe、Mn等金属元素来源于海水。此外,有研究表明微生物在富钴结壳的形成过程中也起着非常重要的作用。富钴结壳的分布及特征受地形、水深、基岩类型、海水水文化学特征、经纬度等多种因素的影响,其主要分布于碳酸盐补偿深度以上、最低含氧带以下、水深800~2500 m的海山、岛屿斜坡和海底高地上,西、中太平洋海山区被认为是全球富钴结壳的最主要产出区。     

西太平洋海山富钴结壳的稀土和铂族元素特征及其意义

为了探讨富钴结壳的稀土和铂族元素是否有相似的形成机制,对西太平洋海山富钴结壳稀土和铂族元素进行了类比研究.结果表明:富钴结壳的∑REY范围为1 433.7×10-6~2 888.0×10-6,其中Ce占到近50%,北美页岩标准化后显示较平坦的稀土模式和显著的Ce正异常特征.根据稀土配分模式及已有的Nd同位素结果,富钴结壳具有亲陆壳属性.富钴结壳具有极高的Pt (115.5×10-9~1 132.0×10-9)、(Pt/Pd)_N和 (Pt/Os)_N值,Ir与Pt及Rh与Pt显示良好相关性.经球粒陨石标准化后显示较一致PGE (platinum-group elements) 配分模式,从Os到Pt逐渐富集,Pd元素强烈亏损.已有的Os同位素研究结果显示物源在地质历史时期从幔源属性向陆源属性变化,但富钴结壳PGE元素内部相对含量仍在一定程度上保持稳定.研究认为:富钴结壳对海水中的稀土清扫具有选择性,Ce的正异常恰恰是结壳对海水稀土中Ce的优先选择造成的,从而导致海水亏损Ce.然而海水中Ce的亏损并未改变新形成富钴结壳的稀土模式,原因是在海洋中存在适量的具有亏损Ce特征的磷酸盐等组分,理论上只需要氧化物类稀土与磷酸盐类稀土消耗的稀土与海水中的补给平衡即可.只是在相关过程中,海洋中氧化物类对稀土的选择更具有主动性,而磷酸盐类表现更多的继承关系.尽管Os同位素显示物源供给发生变化,然而富钴结壳PGE模式相对稳定.因此富钴结壳PGE模式同样可以用富钴结壳对PGE的选择性吸收解释,因富钴结壳优先选择Pt与Ir以及相对排斥Pd和Os,形成了现有独特的PGE模式.      

深海沉积物中碲异常的成因

碲在地球上是一种稀有分散元素，碲在地壳中的丰度很低，仅为1.0ng/g；但碲在富钴结壳、海底多金属结核、党海沉积物和陨石中的丰度异常高。为了查明深海沉积物中碲异常的原因，笔者对比分析了深海沉积物中磁性部分与全岩的碲含量和氦同位素组成。结果显示磁性部分的He含量和3He/4He比值及Te含量较全岩的值明显偏高；3He含量与Te含量同步变化；在3He－Te关系图上，二者具明显的正相关关系。本文首次提出深海沉积物中的碲异常与氦同位素异常一样可能是由宇宙尘注入引起的；海底多金属结核和富钴结壳中的碲异常可能也与宇尘有关。     

太平洋海山成矿系统与成矿作用过程

文中初步探讨了太平洋海山富钴结壳成矿系统的结构与成矿作用过程。海山成矿系统的控矿要素主要包括地质要素和海洋要素,地质要素主要包括海山的形成、迁移、沉降和水道的开合等,海洋要素主要包括大洋温盐环流、最低含氧带(OMZ)、文石溶跃面、碳酸盐补偿深度和海山周围海水的动力情况等。重点分析了海山漂移和沉降、水道开合、最低含氧带变化、大洋环流以及气候变化等要素对富钴结壳成矿的控制作用。海山为富钴结壳成矿提供了一个容矿空间,稳定的基岩,即长期稳定的容矿空间,是富钴结壳成矿的基本条件;海山的形成年龄、海山的迁移和水道的开合决定并改变了富钴结壳的成矿背景条件,促使海山成矿系统发生演化。最低含氧带作为富钴结壳成矿的地球化学障,是直接的矿源层;而海山周边的地形旋涡沟通了最低含氧带与富氧、富铁的深层和底层水,使得最低含氧带中的成矿金属离子得到氧化,进而发生胶体凝聚沉淀,形成富钴结壳。以西太平洋海山成矿系统为例,将该区白垩纪以来富钴结壳成矿作用过程划分为5个阶段:(1)白垩纪—始新世,(2)始新世末—晚渐新世,(3)晚渐新世—中中新世早期,(4)中中新世早期—晚中新世早期,(5)晚中新世早期—现代,其中(2)、(3)阶段有利于发育富钴结壳。     

Noble Gas Isotopic Compositions of Cobalt-rich Ferromanganese Crusts from the Western Pacific Ocean and Their Geological Implications

1 Introduction Submarine metallic mineral resources consist mainly of polymetallic nodules and cobalt-rich ferromanganese crusts. Despite being discovered much later than the former, the latter are becoming one of the most important submarine polymetallic ore resources, because they containmany valuable metallic elements such as Co, platinum group elements (PGE), rare earth elements (REE), Ni and Cu, besides high contents of Fe and Mn (He et al., 2001). The Co-rich crusts are widely distr…     

辽宁宽甸新生代火山岩和地幔包体的稀有气体同位素组成及其演化意义

通过对宽甸新生代碱性玄武岩、地幔包体及辉石巨晶的稀有气体同位素组成的分析，认为不同岩性稀有气体含量的差异反映了岩浆作用过程中轻、重稀有气体的分馏特性，较轻的稀有气体(He、Ne)比较重的稀有气体(Kr、xe)具有更高的活动性和不相容性；该地区上地幔源区具有典型的MORB型源区特征，以辉石巨晶为代表；地幔包体的^3He／^4He值较低，可能是地幔流体交代作用造成的；大陆碱性玄武岩具有与大洋玄武岩截然不同的He同位素组成，反映了大陆区地幔岩浆上升过程中受到了陆壳物质混染。地幔源区^40Ar／^36Ar值为350左右，二辉橄榄岩和碱性火山岩的^40Ar／^36Ar值比大气略高，可能有大气组分的混合。部分样品中有^21Ne、^22Ne、^129Xe、^134Xe和^136Xe相对于大气的过剩现象，是核成因造成的。     

Helium and Argon Isotopic Composition of Cenozoic Alkali Basalts and Mantle-Derived Xenoliths from Kuandian, Liaoning Province, China

The noble gas isotopic composition and content data of 2 alkali basalts, 3 Iherzolite xenoliths and one clinopyroxene megacryst from the Kuandian region have confirmed the occurrence of a fractionation of noble gases during magmatism. Light noble gases such as He and Ne are high in mobility and appear to be incompatible as compared with heavy ones ( such as Kr and Xe). Therefore, light noble gases are abundant in volcanics, especially in the volcanics with bubbles; lherzolite xenoliths have relatively high heavy noble gases. The clinopyroxene megacryst has the lowest abundance of noble gases, probably due to its high P-T origin. Noble gas isotopic composition of the clinopyroxene megacryst reveals that the mantle source beneath the Kuandian area has an MORB-like reservoir with^3 He/^4He ratio of—10 Ra(Ra: atmospheric^3 He/^4He ratio) and^40 Ar/^36 Ar ratio of 345.6. The Iherzolite xenoliths possess moderate^3 He/^4He ratios of 2.59 -4.53 Ra, reflecting the loss of primary helium during rock deformation or metasomatism caused by enriched mantle fluids during the up-lifting. The alkali volcanics have very low^3 He/^4 He ratios(0.47—0.61 Ra),indicating a contribution of radiogenic^4 He, probably having resulted from crust contamination. Most of the samples have excess^21 Ne and^22 Ne as compared with atmospheric neon, but Kr and Xe isotopic compositions are indistinguishable from atmospheric values within uncertainties with only individual samples having excess^129Xe,^134Xeand^136 Xe.     

Helium isotopes in ferromanganese crusts from the central Pacific Ocean

Helium isotopes have been measured in samples of two ferromanganese crusts (VA13/2 and CD29-2) from the central Pacific Ocean. With the exception of the deepest part of crust CD29-2 the data can be explained by a mixture of implanted solar- and galactic cosmic ray-produced (GCR) He, in extraterrestrial grains, and radiogenic He in wind-borne continental dust grains. ⁴He concentrations are invariant and require retention of less than 12% of the in situ He produced since crust formation. Loss has occurred by recoil and diffusion. High ⁴He in CD29-2 samples older than 42 Ma are correlated with phosphatization and can be explained by retention of up to 12% of the in situ-produced ⁴He. ³He/⁴He of VA13/2 samples varies from 18.5 to 1852 R_a due almost entirely to variation in the extraterrestrial He contribution. The highest ³He/⁴He is comparable to the highest values measured in interplanetary dust particles (IDPs) and micrometeorites (MMs). Helium concentrations are orders of magnitude lower than in oceanic sediments reflecting the low trapping efficiency for in-falling terrestrial and extraterrestrial grains of Fe-Mn crusts. The extraterrestrial ³He concentration of the crusts rules out whole, undegassed 4-40 μm diameter IDPs as the host. Instead it requires that the extraterrestrial He inventory is carried by numerous particles with significantly lower He concentrations, and occasional high concentration GCR-He-bearing particles.     

On the origins of GEMS grains

From their birth as condensates in the outflows of oxygen-rich evolved stars, processing in interstellar space, and incorporation into disks around new stars, amorphous silicates predominate in most astrophysical environments. Amorphous silicates were a major building block of our Solar System and are prominent in infrared spectra of comets. Anhydrous interplanetary dust particles (IDPs) thought to derive from comets contain abundant amorphous silicates known as GEMS (glass with embedded metal and sulfides) grains. GEMS grains have been proposed to be isotopically and chemically homogenized interstellar amorphous silicate dust. We evaluated this hypothesis through coordinated chemical and isotopic analyses of GEMS grains in a suite of IDPs to constrain their origins. GEMS grains show order of magnitude variations in Mg, Fe, Ca, and S abundances. GEMS grains do not match the average element abundances inferred for ISM dust containing on average, too little Mg, Fe, and Ca, and too much S. GEMS grains have complementary compositions to the crystalline components in IDPs suggesting that they formed from the same reservoir. We did not observe any unequivocal microstructural or chemical evidence that GEMS grains experienced prolonged exposure to radiation.We identified four GEMS grains having O isotopic compositions that point to origins in red giant branch or asymptotic giant branch stars and supernovae. Based on their O isotopic compositions, we estimate that 1-6% of GEMS grains are surviving circumstellar grains. The remaining 94-99% of GEMS grains have O isotopic compositions that are indistinguishable from terrestrial materials and carbonaceous chondrites. These isotopically solar GEMS grains either formed in the Solar System or were completely homogenized in the interstellar medium (ISM). However, the chemical compositions of GEMS grains are extremely heterogeneous and seem to rule out this possibility. Based on their solar isotopic compositions and their non-solar elemental compositions we propose that most GEMS grains formed in the nebula as late-stage non-equilibrium condensates.     

Ion microprobe isotopic measurements of individual interplanetary dust particles

Ion microprobe measurements of D/H ratios in individual fragments of eight stratospheric dust particles give δD values ranging from ?386 to +2534‰ relative to SMOW. The δD values in five particles far exceed those in terrestrial samples and prove that the samples are interplanetary dust particles (IDPs). The hydrogen isotopic composition is heterogeneous on a scale of a few microns demonstrating that the dust is unequilibrated. Measurements of D/H ratios in conjunction with elemental and molecular ion signals in different fragments of individual IDPs show that a carbonaceous phase, not water, is the carrier of the D enrichments. Previous infrared transmission measurements have shown that IDPs fall into three main spectral classes. Particles from two of those three IR classes show large D/H ratios. Two particles studied from the third class do not. However, one of these contains solar flare tracks and is extraterrestrial. Thus, most, but not all, IDPs contain hydrogen with a non-terrestrial isotopic composition.Carbon isotopic measurements on fragments of three IDPs give ratios similar to terrestrial values and show a largely uniform isotopic composition for a given particle. Small, but significant, differences in δ¹³C of ~40‰ between particles are seen. No correlations between the hydrogen and carbon isotopic compositions are observed.The magnesium and silicon isotopic compositions of fragments of three IDPs are found to be normal within measurement errors.     

新疆坡北杂岩体西端镁铁-超镁铁质岩体成因的稀有气体同位素制约

新疆坡北镁铁-超镁铁质杂岩体由一个辉长岩体以及二十多个超镁铁质侵入体组成,其中坡一超镁铁质岩体稀有气体同位素组成揭示存在地幔柱的贡献。坡北杂岩体西端的坡一、坡四、坡十和坡十四等几个超镁铁质岩体的稀有气体同位素对比分析结果表明,岩浆矿物的³He/⁴He值（0.26~2.79Ra）分布于地壳与地幔值之间,较高的²⁰Ne/²²Ne和较低的²¹Ne/²²Ne值分布于Ne质量分馏线（MFL）和L-K线之间,⁴⁰Ar/³⁶Ar=295~598。³He/⁴He与⁴⁰Ar/³⁶Ar比值揭示坡北杂岩体西端不同超镁铁质岩体形成过程中地幔（柱）、地壳和大气组分的贡献不同,岩体成因也可能不同。其中,坡一岩体具有地幔柱作用的贡献,其他三个岩体的岩石圈地幔及地壳流体组分的贡献较大。岩浆地幔源区由深部地幔柱物质叠加俯冲流体交代的岩石圈地幔物质所组成,大气与地壳物质组分可能由俯冲再循环洋壳带入到岩浆地幔源区以及围岩物质的混入。     

Identification of isotopically primitive interplanetary dust particles: A NanoSIMS isotopic imaging study

We have carried out a comprehensive survey of the isotopic compositions (H, B, C, N, O, and S) of a suite of interplanetary dust particles (IDPs), including both cluster and individual particles. Isotopic imaging with the NanoSIMS shows the presence of numerous discrete hotspots that are strongly enriched in ¹⁵N, up to ∼1300‰. A number of the IDPs also contain larger regions with more modest enrichments in ¹⁵N, leading to average bulk N isotopic compositions that are ¹⁵N-enriched in these IDPs. Although C isotopic compositions are normal in most of the IDPs, two ¹⁵N-rich hotspots have correlated ¹³C anomalies. CN⁻/C⁻ ratios suggest that most of the ¹⁵N-rich hotspots are associated with relatively N-poor carbonaceous matter, although specific carriers have not been determined. H isotopic distributions are similar to those of N: D anomalies are present both as distinct D-rich hotspots and as larger regions with more modest enrichments. Nevertheless, H and N isotopic anomalies are not directly correlated, consistent with results from previous studies. Oxygen isotopic imaging shows the presence of abundant presolar silicate grains in some of the IDPs. The O isotopic compositions of the grains are similar to those of presolar oxide and silicate grains from primitive meteorites. Most of the silicate grains in the IDPs have isotopic ratios consistent with meteoritic Group 1 oxide grains, indicating origins in oxygen-rich red giant and asymptotic giant branch stars, but several presolar silicates exhibit the ¹⁷O and ¹⁸O enrichments of Group 4 oxide grains, whose origin is less well understood. Based on their N isotopic compositions, the IDPs studied here can be divided into two groups. One group is characterized as being “isotopically primitive” and consists of those IDPs that have anomalous bulk N isotopic compositions. These particles typically also contain numerous ¹⁵N-rich hotspots, occasional C isotopic anomalies, and abundant presolar silicate grains. In contrast, the other “isotopically normal” IDPs have normal bulk N isotopic compositions and, although some contain ¹⁵N-rich hotspots, none exhibit C isotopic anomalies and none contain presolar silicate or oxide grains. Thus, isotopically interesting IDPs can be identified and selected on the basis of their bulk N isotopic compositions for further study. However, this distinction does not appear to extend to H isotopic compositions. Although both H and N anomalies are frequently attributed to the survival of molecular cloud material in IDPs and, thus, should be more common in IDPs with anomalous bulk N compositions, D anomalies are as common in normal IDPs as they are in those characterized as isotopically primitive, based on their N isotopes.     

西太平洋海山富钴结壳稀土元素(REE)组成原位LA-ICPMS测定

利用激光剥蚀电感耦合等离子体质谱(LA-ICPMS)微区原位分析方法,对采自西太平洋海山具完整三层结构的富钴结壳样品进行了稀土元素(REE)含量测定,结果表明, 虽然均产于西太平洋海山且均具有明显的三层结构,富钴结壳化学组成受地理位置和沉积环境影响很大。绝大多数西太平洋富钴结壳具有高ΣREE、高LREE/HREE、δCe正异常和δEu基本无异常或微弱正异常的特点, 显示它们主要由正常海水沉积形成。结壳不同层圈之间REE组成有较大的区别, 其原因主要在于其形成环境和矿物组成不同。样品0327稀土元素总量(∑REE)由亮煤层到疏松层到外层逐渐升高,且亮煤层δCe和Y/Ho变化非常大,最大值分别为38.61和105.5,显示该层生长环境较为氧化且相对动荡,而样品0346中三层结构的∑REE都非常高,且变化趋势与0327正好相反,从亮煤层到致密层∑REE有降低的趋势。 亮煤层形成时海水相对较氧化的环境有利于铁锰氧化物的形成和Ce⁴⁺等稀土元素的吸附,导致其中ΣREE较疏松层和外层为高,而后期磷酸盐化导致REE元素的迁移和亏损。在结壳生长剖面上,由最外层到疏松层和亮煤层,δCe呈明显上升趋势,且变化范围趋大,说明该结壳所处的海水环境在由老至新的生长过程中由相对动荡和氧化变为相对平静和还原。     

CCSD中HP-UHP岩石稀有气体同位素地球化学及其对板块折返过程的示踪意义

利用高真空气相质谱系统测定了CCSD中HP-UHP变质岩中主要造岩矿物流体包裹体的稀有气体同位素组成,得出其3He/4He为(0.004~0.775)×10-6,相应R/Ra为0.003~0.553,40Ar/36Ar变化较大,为316.2~11358.8,高于大气40Ar/36Ar(295.5);20Ne/22Ne和21Ne/22Ne分别为9.47~12.4和0.026~0.051,而134Xe/132Xe和136Xe/132Xe分别为0.376~0.484和0.324~0.416,均高于其相应大气值。CCSD中HP-UHP岩石主要造岩矿物的He-Ar、Xe和Ne等同位素组成清楚显示其中流体包裹体主要由地壳变质流体和少量大气饱和水组成,而深源地幔流体组分很低,其中He主要来自地壳,Ar主要由壳源放射性成因40Ar*和少量(平均32.6%)大气Ar混合组成,少量Ne和Xe可能来自地幔。CCSD中HP-UHP岩石具有F40Ar相似文献