陨石氧同位素组成及其地学意义

介绍了各类陨石氧同位素组成的特点,对陨石氧同位素组成的主要成因观点进行了评述,结合地球的原始物质组成,讨论了陨石氧同位素组成的地球科学意义。     

岫岩陨石撞击坑结构高精度地震探测研究

我国的岫岩陨石撞击坑位于辽东半岛北部低山丘陵地区,直径1.8 km,保存完好,已被多方面的证据证实为陨石撞击坑.陨石的撞击和此后的沉积作用在坑内形成了特殊的地球物理场,使坑内与坑外的介质在速度、密度等方面存在差异.本次通过采用反射和折射地震相结合的探测方法,利用陨石撞击所形成的岩石的地震波速度和波阻抗差异,获得了陨石坑...     

沽源超级环形构造与中生代成矿大爆发

由火山喷发、岩浆侵入或陨石撞击作用所形成的环形构造,是地球物质活化迁移的重要场所,对区域成矿过程具有极大的制约意义。在河北省西北部坝上地区,围绕沽源县城一带,早白垩世岩浆岩、布格重力异常及水系沉积物地球化学异常均呈现明显的多级环带分布。这种现象并非尚义-崇礼-赤城深大断裂与乌龙沟-上黄旗岩浆岩带的简单复合叠置,而是以沽源为中心的火山机构的具体表现。该环形构造至少可划分为三个岩浆岩环带,分布着早白垩世（K—Ar100～123Ma）安山质火山-沉积岩和燕山旋回第四期（K—Ar100～138Ma）次粗面岩、次安山岩、二长斑岩、石英正长斑岩等浅成超浅成侵入岩体或岩株,它们的银、铅、锌、镉、铀、钍、钼、砷、锑等元素显著活化和富集。该环形构造控制着蔡家营铅锌矿、张麻井铀钼矿、彭家沟银矿、青羊沟铅锌矿、牛圈银金矿及北岔沟门铅锌银矿的时空定位。若干迹象表明,沽源环形构造可能是白垩纪时期一次陨击事件（因火星和木星之间两颗小行星的碰撞）的结果,这也许是中生代成矿大爆炸的根本诱发机制。     

Impact cratering: The South American record – Part 1

The Earth’s impact record is known to be rather limited in both time and space. There are ca. 190 impact structures currently known on Earth, representing a minor fraction of all the impact events that contributed to the initial formation of our protoplanet, and then to formation and modification of the surface of the planet. Moreover, the distribution of impact structures on Earth is manifestly uneven. One continent that stands out for its relatively small number of confirmed impact structures and impact ejecta occurrences is South America. The limited impact record for this large continent makes a robust case that there is a significant potential for further discoveries. Significant information on the impact record of South America is dispersed in different types of publications (journal articles, books, conferences abstracts, etc.), and in several languages, making it difficult to access and disseminate it among the geoscientific community. We aim to present a summary of the current knowledge of the impact record of this continent, encompassing the existing literature on the subject. It is published in two parts, with the first one covering an up-to-date introduction to impact cratering processes and to the criteria to identify/confirm an impact structure and related deposits. This is followed by a comprehensive analysis of the Brazilian impact structures. The Brazilian impact record accounts for the totality of the large structures of this kind currently confirmed in South America. The second part will examine the impact record of other countries in South America, provide information about a number of proposed impact structures, and review those that already have been discarded as not being formed by impact.     

滇西南发现石英面状变形构造

采自云南省西南部澜沧江中游临景大桥以东约2km、勐戛河下游北岸的岩石样品的薄片中发现了非常清晰的石英面状变形构造(PDFs)。根据伦敦大学矿物岩石与冰物理实验室费氏台(universalstage)测量分析结果、样品所在地地层时代特征和航卫遥感图像特征的综合分析,认为该PDFs属陨击成因,其陨击事件大约发生在白垩/第三纪边界(距今65Ma),所引起的冲击变质作用已接近最高级阶段的高压二氧化硅相,样品位置接近陨击坑的中心。     

Geology of five small Australian impact craters

Here we present detailed geological maps and cross-sections of Liverpool, Wolfe Creek, Boxhole, Veevers and Dalgaranga craters. Liverpool crater and Wolfe Creek Meteorite Crater are classic bowl-shaped, Barringer-type craters. Liverpool was likely formed during the Neoproterozoic and was filled and covered with sediments soon thereafter. In the Cenozoic, this cover was exhumed exposing the crater's brecciated wall rocks. Wolfe Creek Meteorite Crater displays many striking features, including well-bedded ejecta units, crater-floor faults and sinkholes, a ringed aeromagnetic anomaly, rim-skirting dunes, and numerous iron-rich shale balls. Boxhole Meteorite Crater, Veevers Meteorite Crater and Dalgaranga crater are smaller, Odessa-type craters without fully developed, steep, overturned rims. Boxhole and Dalgaranga craters are developed in highly foliated Precambrian basement rocks with a veneer of Holocene colluvium. The pre-existing structure at these two sites complicates structural analyses of the craters, and may have influenced target deformation during impact. Veevers Meteorite Crater is formed in Cenozoic laterites, and is one of the best-preserved impact craters on Earth. The craters discussed herein were formed in different target materials, ranging from crystalline rocks to loosely consolidated sediments, containing evidence that the impactors struck at an array of angles and velocities. This facilitates a comparative study of the influence of these factors on the structural and topographic form of small impact craters.     

The effects of parent-body hydrothermal heating on amino acid abundances in CI-like chondrites

We determined the amino acid abundances and enantiomeric compositions of the Antarctic CI1 carbonaceous chondrites Yamato (Y)-86029 and Y-980115, as well as the Ivuna and Orgueil CI1 carbonaceous chondrites by liquid chromatography with fluorescence detection and time-of-flight mass spectrometry. Y-86029 and Y-980115 both show evidence of parent-body heating (500–600 °C) in addition to aqueous alteration, while Ivuna and Orgueil only show evidence for aqueous alteration. In contrast to Ivuna and Orgueil, which each contain ∼70 nmol/g of amino acids in acid-hydrolyzed, water extracts, both heated Yamato CI meteorites contain only low levels of amino acids that were primarily l-enantiomers of proteinogenic amino acids, indicating that they are likely to be terrestrial in origin. Because indigenous amino acids have been found in meteorites that have experienced metamorphic temperatures of >1000 °C with only minimal aqueous alteration, heating alone is not sufficient to explain the lack of amino acids in Y-86029 and Y-980115. Rather, our data suggest that the combination of heating and aqueous alteration has a profound destructive effect on amino acids in meteorites. This finding has implications for the origins of amino acids and other molecules in the early evolution of our solar system.     

岫岩陨石坑三维Q值层析成像

到2009年为止,世界上已发现176个陨石撞击坑.从20世纪80年代起,中国学者从地质、地球化学和地质钻探角度推断并证实辽宁省岫岩县的一个环形构造为陨石撞击而成,但该坑的深部构造及整体特征仍有待地球物理方法来确认.本文从地震勘探角度利用三维Q值层析成像方法首次对岫岩坑的地震波衰减结构进行了研究,以便对该撞击构造有个整体认识.Q值结构对了解地壳的非弹性性质、地壳介质非均匀性有着重要意义.利用基于吸收特征时间t^*的三维Q值层析成像方法,计算了岫岩坑地震折射方阵的观测数据的振幅谱,并通过拟合振幅谱得到了反映地震波衰减的t^*.利用t^*通过三维Q值层析成像方法获得了该坑的三维Q值结构.结果表明:该陨石坑内从地表到深度100 m的Q值层对应坑内上部107 m厚的湖泊相沉积物,深度100~300 m的Q值层对应坑内下部厚度为188 m的角砾岩堆积透镜体.深度300~700 m的Q值层对应角砾岩堆积透镜体下面的下元古界变质岩系程度较低的撞击破碎层.大约250 m深处的波阻抗界面与地质钻孔的260 m深处的陨石冲击分界面相对应.     

Mineralogy of phyllosilicate-rich micrometeorites and comparison with Tagish Lake and Sayama meteorites

Four phyllosilicate-rich micrometeorites (MMs) were investigated by a synchrotron radiation X-ray diffraction technique and transmission electron microscopy. Three are saponite-rich MMs and one is a serpentine-rich one. In the saponite-rich MMs, we could not find serpentine, and vice versa in the serpentine-rich MM. In the saponite-rich MMs, major constituent minerals are saponite, Fe- and Ni-bearing sulfides, and magnetite. Two saponite-rich MMs contain fine-grained magnesiowüstite-rich aggregates. The aggregates consist of <50 nm polygonal magnesiowüstite coexisting with minor Fe sulfide grains. Their texture, chemical composition, and the result of heating experiments on matrix fragments of the Tagish Lake carbonaceous chondrite strongly suggest that these aggregates were formed by the breakdown of Mg- and Fe-rich carbonate grains when the MMs entered the Earth’s atmosphere. The estimated major mineral assemblage of the saponite-rich MMs before entering the Earth’s atmosphere is very similar to that of the Tagish Lake carbonate-rich lithology, and we suggest that the MMs and the meteorite were derived from similar asteroids. The major mineral assemblage and texture of the matrix of serpentine-rich MM are similar to the matrix of the Sayama CM2 chondrite that experienced heavy aqueous alteration. Chemical compositions of serpentine in the MM suggest that the degree of aqueous alteration of the MM is weaker than that of Sayama. In the MM, cronstedtite does not coexist with tochilinite, which is different from CM2 chondrites that experienced weak to moderate aqueous alteration. However, the possibility that the serpentine-rich MM was derived from the CM chondrite asteroid cannot be ruled out, because tochilinite can be preferentially decomposed during atmospheric entry heating due to its lower decomposition temperature than that of cronstedtite.     

车里雅宾斯克(Chelyabinsk)陨石的岩石矿物特征与冲击变质作用

2013年2月15日,俄罗斯车里雅宾斯克(Chelyabinsk)发生了伴随罕见的空中爆炸的大规模陨石雨事件。本文对3块代表不同冲击变质程度的车里雅宾斯克陨石碎块进行了研究。它们都具有部分熔壳,其中1块仅出现碎裂,1块含有冲击熔融细脉,1块基本由冲击熔融囊和冲击熔脉组成。冲击变质程度最低的样品,代表了该陨石母体小行星的原始岩石矿物学特征:即具有粗粒的岩石结构和均一的矿物化学组成,但仍保留一些残余球粒,表明受到了明显的热变质作用,其岩石类型可划分为5型。铁镁质硅酸盐高的Fe O含量(橄榄石Fa:27.9mol%~28.2mol%,辉石Fs值:23.3mol%~23.7mol%)、以及较低的Fe-Ni金属含量,表明其化学群属于低铁低金属的LL群。我们所分析的样品与前人报导的结果相似,未发现不同岩性的岩屑,表明车里雅宾斯克陨石的原始岩矿特征较为均一。3块陨石碎块中,随着冲击程度的增强,其冲击变质特征依次表现为硅酸盐矿物的破碎、熔长石化更为普遍、陨硫铁与铁镍合金共熔、硅酸盐熔脉的形成、铬铁矿与长石共熔、以及大量熔融囊的发育等。但是,在冲击熔融囊和熔脉中,以及相邻围岩中均未发现高压矿物相。熔脉中的橄榄石晶屑和相邻围岩的橄榄石颗粒表现为化学成分的不均一,在背散射电子图像中呈不同灰度的结构。这与其他强烈冲击变质陨石中橄榄石的林伍德石或瓦茨利石相变相似。该陨石中林伍德石或瓦茨利石的缺失很可能是由于强烈撞击后高温产生的退变质。这也表明车里雅宾斯克陨石的母体小行星可能遭受了非常强烈的撞击事件。