共查询到19条相似文献，搜索用时 500 毫秒
1.
利用地幔橄榄岩包体中平衡矿物对的氧逸度计可以有效限定岩石圈地幔的氧化-还原状态.本文使用中国地质大学(武汉)新购置的WSS-10型常温穆斯堡尔光谱仪对华北地块西北部狼山地区橄榄岩包体的四相矿物开展了铁价态的直接测定.结果显示,斜方辉石Fe3+/∑Fe为0.05～0.11,单斜辉石的为0.16～0.25,尖晶石的为0.16～0.22,橄榄石为0.利用橄榄石-斜方辉石-尖晶石氧逸度计,获得狼山地区岩石圈地幔氧逸度为FMQ-0.82至FMQ-0.39(均值为FMQ-0.65).该值略高于依据电子探针测试数据计算获得的氧逸度值(FMQ-1.49至FMQ-0.8,均值为FMQ-1.25),造成这一差异的原因可能是后者忽略了尖晶石晶格中Fe3+过剩和阳离子空位导致的非化学计量比.与全球克拉通岩石圈地幔氧逸度值(均值为FMQ-0.35)相比,华北地块西北缘狼山地区岩石圈地幔整体表现为较还原状态,推测与深部地幔低fO2熔体上升交代有关. 相似文献
2.
撞击地层学及其研究进展 总被引：2，自引：0，他引：2
地质历史中的地外物体撞击地球事件可在撞击点、近源区和远源区分别形成撞击坑熔融岩体、近源溅射岩席及海啸沉积和远源溅射层等一系列撞击地层层序。撞击地层有其独特的物理学和化学特征,与正常沉积作用、火山喷发和板块碰撞等成因的地层显然有别。通过对撞击地层层序的时空变化、所包含的撞击成因矿物、撞击微球粒和微玻璃陨石以及古生物和地球化学异常等的研究,可以了解撞击事件的发生频率、幅度和撞击天体的性质等,也为探索生物和地球环境的灾难性变化及其起因提供了新的思路。 相似文献
3.
富Ca,Al包体、球粒和蠕虫状橄榄石集合体都是早期星云事件的产物。本文探讨了4个富橄榄石的富Ca,Al组分集合体的矿物岩石学特征,并对它们进行了对比。矿物岩石学特征表明含橄榄石边的富尖晶石-辉石型包体和富Ca,Al组分蠕虫状橄榄石集合体都属于星云直接凝聚的产物,而富钙长石-橄榄石型包体(POI)和富Ca,Al组分球粒经历过熔融结晶过程。矿物模式组成表明POI包体和富Ca,Al组分球粒可能是认识典型富Ca,Al包体与球粒之间相互关系的钥匙。蠕虫状橄榄石集合体GRV022459-2C1中尖晶石普遍具有高的FeO含量,表明其蚀变发生于高氧逸度的星云环境。球粒与粗粒富Ca,Al包体可能属于同一热事件的产物,粗粒富Ca,Al包体形成于富Ca,Al矿物富集的区域,Mg,Fe质硅酸盐球粒形成于富Ca,Al矿物缺失的区域,POI包体和富Ca,Al组分球粒可能形成于上述两个区域之间的过渡区域。 相似文献
4.
氧逸度可以用于定量描述一个体系的氧化还原状态,是地球科学非常重要的一个热力学指标。早期地球的氧逸度及其变化趋势的重建,对大气圈、水圈、生物圈乃至整个地球的起源和演化具有重要的科学意义,也是地球科学长期探索的重要目标。锆石提供了地球上已发现的最古老天然样品,几乎是目前研究早期(冥古宙)地球的唯一可靠对象。近年来的研究发现,锆石中Ce的含量对其母岩浆体系的氧逸度很敏感,并由此发展出了锆石的Ce氧逸度计。这一技术对认识早期地球的氧化还原状态十分关键。文章对锆石Ce氧逸度计进行了简单介绍,进而对早期地壳和地幔的氧化还原状态进行了综合评述。在此基础上,对早期地球几个重要圈层(大气圈、大陆地壳和上地幔)氧逸度的演化及相互间的耦合关系进行了讨论。 相似文献
5.
《地球化学》2020,(1)
地球是一个"氧化性"的星球。在太阳系所有行星中,只有地球大气中含有高浓度的O_2(约占21%)。研究表明,地球演化的早期,其大气组成与火星等类地行星相似,都是以CO_2为主,O_2含量可以忽略不计。在大约24-21亿年前,地球大气中O_2含量突然大幅度升高,一度超过现今O_2含量的1%,而后又在中元古代回落到现今O_2含量的0.1%以下。沉积物中氧化还原敏感元素的含量变化显示,大约6.3亿年前雪球地球结束之后,地球大气中的O_2含量再次大幅度升高至20%左右,而后在显生宙经历一系列复杂变化并最终演化至现今的水平。Re/Os比值显示,硅酸盐地球的氧逸度远高于月球,也高于火星。考虑到月球与地球分异发生在45亿年前,月球的低氧逸度暗示地球早期的氧逸度可能也较低。可以影响地球氧逸度的元素主要有O、H、Fe、S和C等。控制地球氧逸度变化的主要过程包括:核幔分异、板块俯冲和火山喷发去气等。在核幔分异以前,金属Fe可能是控制硅酸盐地球及其表生环境低氧逸度的关键因素。核幔分异过程中,Fe是控制氧逸度变化的关键元素。核幔分异将金属Fe与铁氧化物分开,造成地幔Fe~(3+)/Fe~(2+)比值升高。尤其是在下地幔,Fe~(2+)在高压下发生歧化反应,形成金属Fe和Fe~(3+)。其中Fe~(3+)赋存在布里奇曼石中,导致下地幔氧逸度低。在板块俯冲过程中,当有板片进入下地幔时,布里奇曼石会因体积补偿,被运移到上地幔,并发生分解,释放出Fe~(3+),导致周围地幔氧逸度的升高。但是,V/Sc和Zn/Fe等元素比值则显示在过去30多亿年以来,地幔的氧逸度变化不大,可能与上、下地幔间氧化还原缓冲层或者是上述元素比值对氧逸度不够敏感有关。在地球演化早期,金刚石是最早形成的矿物。由于金刚石的密度在上地幔高于地幔橄榄岩熔体,而在下地幔小于地幔橄榄岩熔体,因此在岩浆海阶段,金刚石倾向于在上地幔底部富集,成为一个富金刚石的储层。在板块俯冲阶段,这些金刚石会被布里奇曼石分解所释放的Fe~(3+)所氧化,形成富碳酸盐和CO:的层位,同时起到稳定上地幔氧逸度的作用。俯冲带地幔橄榄岩和岛弧火山岩的氧逸度均高于板内环境,因此一般认为板块俯冲会导致氧逸度升高。在板块俯冲过程中,氧逸度主要受到Fe和H_2O(水分解释放出H_2)的控制。蚀变大洋岩石圈中含有大量的H_2O,板块俯冲过程中脱水会导致地幔楔蛇纹石化。蛇纹石化过程会形成磁铁矿,释放出味,使局部在短时间内氧逸度降低。但是,由于H_2很容易逸散到大气中,而磁铁矿则保留在地幔楔中,其结果导致岩石中Fe~(3+)/Fe~(2+)比值升高,从而在发生部分熔融时形成高氧逸度岩浆。板块俯冲对氧逸度的影响是多方面的,还与俯冲板块的年龄、沉积物的性质等有关。对于富含有机物的沉积物俯冲过程,C是主要的氧逸度控制元素。在板块俯冲的浅部,有机物分解,释放出CH_4等还原性气体,造成上覆岩石圈氧逸度下降。富含铁锰结核等氧化性沉积物的俯冲则可以导致地幔楔氧逸度的升高,这一过程中Fe和Mn是控制氧逸度的主要元素。火山喷发可以释放出CH_4、CO_2、H_2S和SO_2等气体,也可以影响大气中O_2的含量。有研究认为,火山气体中的H_2S随岩浆房压力增加而增加,SO_2则随压力的增加而减少,因此岩浆房压力可以影响其排气的氧化-还原性,进而影响大气的O_2含量。一种观点认为,正是由于太古宙末期大量出现陆相火山岩,导致了大氧化事件,在这一模型中,S是控制氧逸度的关键。氧逸度对多种成矿作用均具有重要的控制作用。其中,斑岩铜金矿床的形成往往与高氧逸度的埃达克岩有关。这是由于当岩浆的氧逸度高于AFMQ+1.5时,岩浆中S主要以硫酸盐的形式存在。由于硫酸盐在岩浆中的溶解度远远高于硫化物,因此,在俯冲洋壳部分熔融过程中形成的高氧逸度埃达克质岩浆可以熔出更多的亲硫元素,有利于成矿。锡矿床的形成则往往与还原性岩浆有关。这是因为在高氧逸度岩浆中,Sn主要呈Sn~(4+),易于在岩浆结晶早期进入矿物中;而在还原性岩浆中,Sn主要以Sn~(2+)形式存在,表现为不相容元素,倾向于在岩浆中富集,并在岩浆期后热液阶段富集成矿。其他氧化还原敏感元素,如U、V、Mo、Re、Sb和Fe等,可以在表生过程中富集,有利于进一步富集成矿。 相似文献
6.
氧逸度是定量表示一个体系氧化还原能力的指标，反映了体系中氧气的分压或者逃逸能力。在地球科学中，它反映了岩石和矿物中变价元素的氧化还原状态，指示了不同岩石矿物氧化性/还原性的相对强弱。相同岩石矿物不同氧逸度可以导致其物理化学性质发生大的改变，因此在实验地球科学中准确控制并监测高温高压实验条件下的氧逸度具有非常重要的意义。本文从实验技术角度出发，首先介绍了活塞圆筒和多面砧高压装置中利用双胶囊技术在不含水和含水体系中控制氧逸度的方法、原理、装置和注意事项；接着描述了用过渡金属合金固溶体和惰性金属合金作为氧传感器原位测量氧逸度的原理、注意事项和地质应用，然后展示了氧离子固体电解质法控制和监测氧逸度的原理、装置和局限，提出了可能的改进方法。目前由于技术限制，氧逸度在高压实验中的控制和监测方法还不成熟，导致其对矿物和岩石物理化学性质的影响极可能被低估甚至错估。因此积极研究发展并推动高压下氧逸度的控制和监测技术非常重要且必要。 相似文献
7.
撞击作用发生在太阳系形成和演化的所有阶段,是最基本的地质过程之一.陨石可以从微观尺度记录下这些重要的过程.在所有陨石族群中,L 群普通球粒陨石保留了最完备的冲击变质记录,对撞击发生的时间、冲击过程中的物理条件提供了重要制约.矿物学证据表明,在太阳系形成 100 Ma 内,L 群陨石母体可能发生一次撞击裂解事件,并在随后重组.4. 48 Ga左右,原始小行星带经历大范围的撞击作用,这一事件也记录于L群普通球粒陨石中,可能是由月球大撞击事件溅射的大量碎屑进入到原始主小行星带引起.约800 Ma,包括L群陨石母体在内的内太阳系部分天体经历了同时期撞击事件,可能由这一时期裂解的大质量小行星产生的溅射物引发.L群陨石母体在～465 Ma发生撞击裂解,这一事件在 L 群陨石中保留了丰富的矿物学、年代学记录,并在地球全球奥陶纪地层发现相关信息.综合与该事件相关的所有L群陨石冲击变质特征,本文认为该裂解事件是由一颗大直径(18～22 km)石陨石质小行星,以较低速率(5～6 km/s)撞击导致.同位素年代学数据表明,L 群普通球粒陨石母体很可能未受到晚期大撞击事件的影响,这难以用L群陨石母体过小予以解释.可能的原因有:① L群普通球粒陨石母体在原始主小行星带分布非常有限,导致其受到晚期大撞击事件影响的概率不高;② 晚期大撞击事件对原始主小行星带的影响可能并没有之前估计的那么严重,一个持续时间更长但更加温和的撞击模型更加符合现阶段的观察. 相似文献
8.
地质记录中的微球粒 总被引：1，自引：0，他引：1
地质记录中的微球粒根据成因可以分为宇宙尘、地外物体撞击成因微球粒、火山成因微球粒、生物成因微球粒、沉积作用微球粒和现代微球形飞灰等。宇宙尘含有丰富的宇宙物质,出现Fe、Ni核心和方铁矿等,具有宇宙尖晶石和宇宙不丰富的元素的亏损是判断宇宙尘的关键特征。撞击事件可以产生近源区的撞击熔融玻璃球和远源区的撞击汽云凝结球两类微球粒,常与其他撞击成因矿物伴生。火山微球粒是在低粘稠度的岩浆岩喷发形成的玻璃质火山灰中,有球形、液滴形和哑铃形的微颗粒。这三种成因的微球粒在各种地层中的赋存对于地层对比和地史事件研究中有着非常重要的意义,为判断和研究不同的地质事件提供了一个很好的媒介,因此长期以来一直是微球粒研究的主要对象。另外,在现代工业生产过程中也可以产生大量微球形飞灰,这些飞灰经常包含非常复杂的表面纹饰和独特的化学组成,比如高的ZnO含量等。 相似文献
9.
本文研究了2个富钙长石-橄榄石型包体和2个富黄长石-尖晶石型和富尖晶石-辉石型包体（分别来自宁强和南极格罗夫山碳质球粒陨石）的矿物岩石学特征,并对它们进行了对比。富钙长石-橄榄石型包体的矿物模式组成具有富橄榄石和缺失黄长石的特征,其可能是球粒和典型难熔包体之间的中间产物,是认识它们之间相互关系的钥匙。矿物岩石学特征表明富黄长石-尖晶石型和富尖晶石-辉石型包体可能是星云直接凝聚的产物,而富钙长石-橄榄石型包体经历过熔融结晶过程。富钙长石-橄榄石型包体的初始物质可能是富Al的球粒或含难熔组分的蠕虫状橄榄石集合体。矿物化学组成对比研究发现,GRV 022459-RI6中的尖晶石具有最富FeO的特征,表明包体的蚀变可能发生在高氧逸度的星云环境。 相似文献
10.
近年来,人们取得了一系列地外灾变事件的证据,特别是铱异常和微球粒的发观,被人们认为是天体撞击地球的直接证据。本文仅对微球粒作些粗浅讨论。 相似文献
11.
During their deceleration through the Earth's atmosphere, meteoritic materials, i.e., interplanetary dust particles, micrometeorites and meteorites, experience thermal shocks which may alter their pristine mineralogy, texture or chemical characteristics. Among these changes, one of the most ubiquitous is the formation of spinels resulting from partial melting and subsequent crystallization of the meteoritic material. These “cosmic spinels” differ from terrestrial spinels by their high Ni and Fe3+ contents and show large variations in composition. In order to better understand the factors controlling their chemistry, pulse-heating experiments simulating atmospheric entry of extraterrestrial objects were carried out using Orgueil samples as proxies of meteoritic material. Covering a large range of experimental conditions (temperature 500°C < T <1500°C, duration: 5 s < t < 120 s, and oxygen fugacity: −0.68 < log fO2 < −8), this work shows (1) that the whole range of composition of cosmic spinels analyzed so far at the micrometer scale in fine-grained and scoriaceous micrometeorites, in cosmic spherules or in the fusion crust of several stony meteorites can be reproduced, and (2) that these compositional changes can be expressed as a function of temperature, time and oxygen fugacity.We also show that, due to their fast crystallization kinetics, cosmic spinels can record through their composition, i.e., Al2O3 contents and FeO/Fe2O3 ratio, the diverse conditions of the atmosphere crossed by the extraterrestrial object during its fall towards the Earth's surface. Chemistry of cosmic spinels is thus a powerful tool for constraining the entry conditions in the Earth's atmosphere of any extraterrestrial object, including altitude of deceleration, entry angle and incident velocity. These in turn, may provide valuable information on the origin of the extraterrestrial material. 相似文献
12.
本文报道了攀枝花钒钛磁铁矿含矿岩体边缘岩相带中的苦橄玢岩和岩体中淡色辉长岩的锆石微量元素特征。结果表明二者所含锆石都具有明显的Ce正异常和Eu负异常,以及轻稀土元素亏损和重稀土元素富集的特征,其Th/U比值为0.35～3.23,都属于典型的岩浆锆石。本次研究利用最新实验标定的锆石氧逸度计对苦橄玢岩和淡色辉长岩的氧逸度进行了估算。估算结果表明苦橄玢岩和淡色辉长岩均具较高的氧逸度,分别为QFM+0.3～QFM+2.5和QFM+0.7～QFM+3(QFM为石英-铁橄榄石-磁铁矿缓冲剂)。苦橄玢岩作为来自深部岩浆房侵入到攀枝花主岩体的富橄榄石"晶粥体",其高氧逸度的特征反映出攀枝花岩体的原生岩浆以及地幔源区是相对氧化的,而导致这一结果的原因很可能与古老俯冲事件导致的地幔交代作用有关。通过地幔柱-岩石圈相互作用,在较高氧逸度下发生部分熔融形成了铁质苦橄岩及其堆晶作用产物苦橄玢岩。此外,淡色辉长岩的氧逸度也显示出较高的特征,这说明这种氧化的特征很可能是贯穿了整个成岩过程的,对钒钛磁铁矿成矿,特别是导致铁钛氧化物早期结晶起到了不可忽视的作用。 相似文献
13.
Clément Suavet Carole Cordier Luigi Folco Corinne Sonzogni 《Geochimica et cosmochimica acta》2011,75(20):6200-6210
In order to identify the parent bodies of cosmic spherules (melted micrometeorites) with porphyritic olivine (PO) and cryptocrystalline (CC) textures, we measured the oxygen isotopic composition of 15 giant (>800 μm) cosmic spherules recovered in the Transantarctic Mountains, Antarctica, with IR-laser fluorination/mass spectrometry, and we conducted a characterization of their petrographic and magnetic properties. Samples include 6, 8 and 1 spherules of PO, CC and barred olivine (BO) textural types, respectively. Eleven spherules (∼70% of the total: 4/6 PO and 6/8 CC, and the BO spherule) are related to ordinary chondrites based on oxygen isotopic compositions. Olivines in ordinary chondrite-related spherules have compositions Fa8.5-11.8, they are Ni-poor to Ni-rich (0.04-1.12 wt.%), and tend to be richer in CaO than other spherules (0.10-0.17 wt.%). Ordinary-chondrite related spherules also have high magnetite contents (∼2-12 wt.%). One PO and one CC spherules are related to previously identified 17O-enriched cosmic spherules for which the parent body is unknown. One CC spherule has an oxygen isotopic signature relating it to CM/CR carbonaceous chondrites. The majority of PO/CC cosmic spherules derive from ordinary chondrites; this result exemplifies how the texture of cosmic spherules is not only controlled by atmospheric entry heating conditions but also depends on the parent body, whether be it through orbital parameters (entry angle and velocity), or chemistry, mineralogy, or grain size of the precursor. 相似文献
14.
Cécile Engrand Kevin D. McKeegan Gregory F. Herzog Laurence E. Nyquist 《Geochimica et cosmochimica acta》2005,69(22):5365-5385
Large, correlated, mass-dependent enrichments in the heavier isotopes of O, Cr, Fe, and Ni are observed in type-I (metal/metal oxide) cosmic spherules collected from the deep sea. Limited intraparticle variability of oxygen isotope abundances, typically <5‰ in δ18O, indicates good mixing of the melts and supports the application of the Rayleigh equation for the calculation of fractional evaporative losses during atmospheric entry. Fractional losses for oxygen evaporation from wüstite, assuming a starting isotopic composition equal to that of air (δ18O = 23.5‰; δ17O = 11.8‰), are in the range 55%-77%, and are systematically smaller than evaporative losses calculated for Fe (69%-85%), Cr (81%-95%), and especially Ni (45%-99%). However, as δ18O values increase, fractional losses for oxygen approach those of Fe, Cr, and Ni indicating a shift in the evaporating species from metallic to oxidized forms as the spherules are progressively oxidized during entry heating. The observed unequal fractional losses of O and Fe can be reconciled by allowing for a kinetic isotope mass-dependent fractionation of atmospheric oxygen during the oxidation process and/or that some metallic Fe may have undergone Rayleigh evaporation before oxidation began.In situ measurements of oxygen isotopic abundances were also performed in 14 type-S (silicate) cosmic spherules, 13 from the Antarctic ice and one from the deep sea. Additional bulk Fe and Cr isotopic abundances were determined for two type-S deep-sea spherules. The isotopic fractionation of Cr isotopes suggest appreciable evaporative loss of Cr, perhaps as a sulfide. The oxygen isotopic compositions for the type-S spherules range from δ18O = −2‰ to + 27‰. The intraspherule isotopic variations are typically small, ∼5% relative, except for the less-heated porphyritic spherules which have preserved large isotopic heterogeneities in at least one case. A plot of δ17O vs. δ18O values for these spherules defines a broad parallelogram bounded at higher values of δ17O by the terrestrial fractionation line, and at lower values of δ17O by a line parallel to it and anchored near the isotopic composition of δ18O = −2.5‰ and δ17O = −5‰. Lack of independent evidence for substantial evaporative losses suggests that much of this variation reflects the starting isotopic composition of the precursor materials, which likely resembled CO, CM, or CI chondrites. However, the enrichments in heavy isotopes indicate that some mixing with atmospheric oxygen was probably involved during atmospheric entry for some of the spherules. Isotopic fractionation due to evaporation of incoming grain is not required to explain most of the oxygen isotopic data for type-S spherules. However spherules with barred olivine textures that are thought to have experienced a more intense heating than the porphyritic ones might have undergone some distillation. Two cosmic spherules, one classified as a radial pyroxene type and the other showing a glassy texture, show unfractionated oxygen isotopic abundances. They are probably chondrule fragments that survived atmospheric entry unmelted.Possible reasons type-I spherules show larger degrees of isotopic fractionation than type-S spherules include: a) the short duration of the heating pulse associated with the high volatile content of the type-S spherule precursors compared to type-I spherules; b) higher evaporation temperatures for at least a refractory portion of the silicates compared to that of iron metal or oxide; c) lower duration of heating of type-S spherules compared to type-I spherules as a consequence of their lower densities. 相似文献
15.
地球的起源与演化研究进展 总被引：3，自引：2，他引：3
地球科学在研究远古地球的形成与演化方面积累了越来越多的证据 ,人类对于太空的观测程度也不断提高 ,加深了对类地行星的认识 ,取得了重要的成果。太阳系中的火星和金星可能存在已经绝灭了的生命。慧星和小行星对地球的多次撞击有能力导致严重的环境效应及生命大灭绝。行星的演化可能有两种模式 :冷的星团加热及热的星云冷却。火星上存在与地球壳体非常相似的沉积岩 ,说明有流动水存在的可能。较高地热的太古代地壳热流输出被认为是认识地壳构造特性的关键。晚太古代会聚与离散大陆边缘的对比研究表明太古代板块运动与年轻的板块构造旋回在样式及幕次方面都没有根本的区别。元古代大陆的增生是由于元古代源于地幔的板块构造及产生于地幔的热柱构造导致新生成分的加入而造成的。裂谷、盆地、推覆及伸展、火山侵入作用是显生宙大陆增生的主要因素。 相似文献
16.
Ferric/ferrous ratios have been used to estimate the oxygen fugacity of lavas erupted in 1984 on Mauna Loa Volcano, Hawaii. Rapidly quenched lavas erupted close to vents are less oxidized than rapidly quenched lavas scooped from lava flows several kilometers away from the vents. These results demonstrate that sampling is of critical importance in determining the oxidation state of lava. The oxidation state of the vent lavas, below or at magnetite–wüstite (MW), is significantly lower than that previously reported for Hawaiian lavas (~FMQ). Similarly, rapidly quenched lavas from the ongoing Kilauea eruption and Loihi seamount, all have oxygen fugacities that are close to MW and on the low side of the range previously reported for Hawaiian lavas. From this we conclude that the initial oxygen fugacity of parental Hawaiian magmas is close to MW, not FMQ, and that previous estimates of the oxidation state of Hawaiian lavas may have been too high. This implies that the plume source of these magmas is also at or below MW, but not as reduced as the mantle source of mid-ocean ridge basalts. Additionally, Mauna Loa lavas appear to be slightly more reduced than Kilauea or Loihi lavas, perhaps indicating heterogeneous oxidation within the Hawaiian plume. 相似文献
17.
PP3超镁铁岩主要岩石类型有纯橄岩和石榴石橄榄岩,两者为渐变,主要矿物为橄榄石、铬尖晶石、石榴石、单斜辉石和斜方辉石.铬尖晶石的Cr#[Cr/(Cr+Mg) ×100]从51~89变化,TiO2和MnO2值分别低于0.26%和0.46%.铬尖晶石矿物表现为4期次演化的特点,反映了从岩浆期、榴辉岩相、角闪岩相和绿片岩相演化特征.随着超镁铁岩的演化,铬尖晶石表现为Cr#不断增大,而Mg#[Mg×100/(Mg+Fe2+) ]不断减少、氧逸度不断增加的过程.PP3铬尖晶石反映了地幔来源,为大陆岩石圈超镁铁岩特征,后期随折返而演化.从石榴石与铬尖晶石相互转变过程看出,PP3超镁铁岩经历了深度加大的过程,超镁铁岩曾经到达100km以上的岩石圈地幔深处.在绿片岩相-绿片角闪岩相变质过程中,铬尖晶石中Cr、Mg和Al减少,Fe相对增加,产生富Cr尖晶石变质作用样式.晚期剪切变形等次生变化影响了铬尖晶石矿物成分. 相似文献
18.
Hiroshi Nagasawa Kazuo Yamakoshi Tadashi Shimamura 《Geochimica et cosmochimica acta》1979,43(2):267-272
The possible existence of meteoritic spherules was investigated among several silicate spherules separated from oceanic sediments and analyzed by means of INAA (instrumental neutron activation analysis).A 0.72 mg glassy spherule was found to have uniform enrichment of 4 ~ 5 for the refractory REE (rare earth elements) and Sc with substantial depletion of Ce relative to chondritic abundances. This implies that this spherule is meteoritic in origin and that the enrichment of refractory elements was established by high temperature heating in a high O/H environment, possibly at the time of entering the Earth's atmosphere.The other three analyzed spherules showed major and trace element abundances that are consistent with an origin in the oceanic environment. 相似文献
19.
Experimental studies, performed under oxidized conditions (fO2 > QFM + 2, where QFM is quartz–fayalite–magnetite oxygen buffer), have shown that Rh, Ru, Ir and Os are strongly compatible with Cr spinel, whereas empirical studies of Cr spinels from ultramafic–mafic rocks suggest that the experimental results may overestimate the partition coefficients. We report laser-ablation inductively coupled plasma mass spectrometry (LA-ICP-MS) analyses of platinum-group elements (PGE), Au and Re abundances in Cr spinels from the Ambae volcano, Vanuatu (fO2 = QFM + 2.5), the Jimberlana layered intrusion, western Australia, and the Bushveld complex, South Africa (fO2 ～ QFM). The results show that Rh and IPGEs (Iridium-group PGE; Ru, Ir, Os) partition strongly into the Cr spinels that crystallized from the oxidized Ambae lavas whereas most of the Cr spinels from the more reduced Jimberlana layered intrusion and the Bushveld complex contain no detectable PGE, Au or Re, with exception of ～10 ppb of Ir in some Jimberlana Cr spinels. In the Ambae Cr spinels, Rh, Ru and, to lesser extent Os, are positively correlated with Fe3+, Ni and V. The homogeneous distribution of Rh and IPGEs in LA-ICP-MS time-resolved spectra indicates that these elements are in solid solution in Cr spinels. Pt–Fe alloys occur as inclusions within the Ambae Cr spinels, which indicate that the Ambae melt was saturated with Pt.Our results show that partitioning of Rh, Ru and Ir into Cr spinels increases with increasing oxygen fugacity, which suggests that the high concentrations of these elements in the Ambae Cr spinels are due to the high oxygen fugacity of the host magma. Therefore, Cr spinels may play an important role in controlling the concentrations of Rh and IPGEs during fractional crystallization of oxidized ultramafic–mafic magmas and during partial melting of oxidized arc mantle. 相似文献