吉林陨石的形成和演化过程

在对吉林陨石进行多学科综合研究所取得的成果基础上,我们对吉林陨石的形成演化过程作了如下讨论:(1)太阳星云的凝聚过程:根据吉林陨石的凝聚和固化年龄和矿物的组合,探讨了太阳星云凝聚的过程;(2)吉林陨石母体的热变质过程:从稀有气体的丢失,全岩化学成分的特征,稀土元素的自纯化过程和橄榄石、斜方辉石成分的稳定性,讨论了热变质过程的特征;(3)吉林陨石母体的冷却过程:根据镍纹石的镍含量和宽度,还根据矿物中Ar和裂变径迹的保存性,分析了吉林陨石母体的冷却史;(4)吉林陨石母体的破碎和宇宙线照射历史:根据对宇宙成因He3、Ne20,21,22、Ar38、Na22、Al26、Mn54、Mn53和Co60的测定结果,提出了吉林陨石的两阶段照射历史的模式。第一阶段的吉林陨石母体,年龄10—11my,r=10m,确定了各样品在母体中的相对位置;第二阶段的吉林陨石母体,年龄0.3—0.5my,r=80—90cm确定了各样品的埋藏深度及通过大气层后的烧失量;(5)吉林陨石的降落过程:讨论了吉林陨星在太阳系空间和大气层中的轨道及降落过程。      

我国某些球粒陨石及中铁陨石稀有气体的同位素丰度

本文测定了剑阁球粒陨石、岩庄球粒陨石、亳县球粒陨石及渭源中铁陨石和新近降落的东乌珠穆沁中铁陨石的稀有气体同位素丰度，根据He、Ne及Ar的测定结果计算宇宙射线暴露年龄，剑阁、岩庄及亳县球粒陨石的宇宙射线暴露年龄分别为5．8Ma、2．5Ma及38．0Ma，东乌珠穆沁及渭源中铁陨石分别为172Ma及17Ma．     

宁强陨石（CV3）稀有气体的研究

宁强陨石的岩石学、矿物学及化学组成的研究表明,宁强陨石属于异常的CV3碳质球粒陨石,稀有气体和宇宙射线暴露年龄的测定结果与岩石学及化学组成的研究结果是一致的,宁强陨石的宇宙射线暴露年龄为42.2Ma,在CV3球粒陨石中是最高的,U/Th-4He及40K-40Ar气体保存年龄分别为4170±160Ma和4260±70Ma,这与碳质球粒陨石的气体保存年龄为4200Ma是一致的.     

陨石宇宙成因核素的研究

本文概括地介绍了吉林陨石宇宙成因核素的研究。特别对吉林陨石Ⅰ号的四个深度样品的CO60深度分布和样品的定位作了详细的描述。最后也讨论了吉林陨石的多重暴露历史。      

安徽亳县球粒陨石的铅同位素研究

本文报道了安徽亳县LL4型球粒陨石的全岩、球粒、橄榄石、辉石和陨硫铁的铅同位素比值,以及上述部分样品的铀、钍、铅的含量.由陨石的铅-铅等时线求得的年龄为45.3±0.2亿年,这是安徽陨石母体的形成年龄.而南安徽陨石的内部等时线求得的年龄为44.4±0.2亿年,此年龄暗示着安徽陨石母体在形成后的大约1亿年以前产生过局部或全部的熔融.从安徽陨石的铀-铅一致曲线图解中得到的上交点年龄为45.4±0.2亿年,此与陨石母体形成的铅-铅年龄一致.而下交点的年龄为4亿年,这可能意味着在较近期内安徽陨石又经历了一次热扰动(如热冲击).全岩、球粒和陨硫铁都呈现出过剩的放射性成因铅,这与陨石经受过热事件有关.      

我国某些普通球粒陨石金属相的元素分布

本文用仪器中子活化分析法测定了我国不同化学群的吉林(H₅),信阳(H₅)、肇东(L₅)、广饶(L_6-5)和东台(LL₆)等普通球粒陨石金属相的Fe、Ni、Co、Cu、Cr、Mn、Ga、Ge、Ir、Au和As含量.每个陨石的金属相按粒径分为>20目.20—40目.<40目等.根据这些结果,讨论了元素的分布规律和分馏趋势以及决定金属相组成的作用过程.      

吉林陨石的熔融实验研究及其在地球化学中的应用

组成地球的初始物质很可能是IAB铁陨石及H群球粒陨石,非均匀吸积形成地球以后,除由岩浆分异作用使幔中金属-硫化物下沉到原始地核外,在还原条件下还有部分Fe是由橄榄石中的FeO还原为Fe0而提供的并加入于地核内.对于大的陨石母体,由于内部加热或其表面受冲击加热而发生熔融和岩浆分异,导致形成某些铁陨石及无球粒陨石或7型岩石类型的球粒岩石.实验产物中的Fe-Ni-S相可作为判别宇宙球粒的标志之一.      

地外撞击球粒的成因探讨：以K／T界面事件为例

本文对KTB地层中富含尖晶石的地外撞击球粒的成份、矿物组成、构造特点等进行了系统研究,通过陨石消熔模拟实验的分析,以及陨石消融成因模式和撞击汽云凝聚成因模式的对比研究,认为该类球粒在成因上既有消融成因的球粒,又有撞击汽云凝聚成因的球粒,并且可能同时存在另外一种成因机制的球粒．     

未分群铁陨石及其硅酸盐包体的研究

本文对Guin陨石进行了化学、矿物学和岩石学方面的研究,表明Guin是一块含有45μg/gGa和186μg/g Ge的难于分类的铁陨石,它是具有异常高镍含量(92.5mg/g)的粗八面体陨铁。它还包含有6±3vol.％硅酸盐包体。包体的组成类似于球粒陨石冲击而成的融体玻璃。因此,我们认为Guin是球粒陨石母体冲击熔融而形成的集合体。      

不是雨的“雨”

陨石雨陨石雨不是雨,它也与气象学无关,只是一个天文学名词。它是指大量陨石体碎块陨落在地球上某一地区的现象。其成因是由于体积较大的流星(亦即“陨星”、“陨石”)体,在陨落的过程中,因其本身结构和组成的不均匀性,在高热、摩擦的作用下,不断地分裂,最后形成许多碎块散落到地面上。不过,在习惯上,人们只是把散落数量达到一定规模的才称为“陨石雨”。例如,1976年3月8日,一块陨石闯入地球大气层,发生燃烧爆炸后降落在吉林市约500平方千米的范围内,这就是举世罕见的“吉林陨石雨”。吉林市博物馆在收集陨石标本的基础上,建成了世界上惟一…     

信阳陨石热历史与原始氩特征

信阳陨石于1977年12月1日18时57分, 陨落在我国河南省信阳县肖王公社。陨落后, 破裂为X-Ⅰ(48kg)及X-Ⅱ(27.5kg)两大块和几小块碎屑。陶克捷等对该陨石做过化学组成、矿物组分及结构特征研究, 指出属H6型。本文试图根据40Ar/39Ar快中子活化资料及原始捕获氩同位素特征, 探讨信阳陨石的演化特点。      

Chemical composition measurements of the atmosphere of Jupiter with the Galileo Probe mass spectrometer.

The Galileo Probe entered the atmosphere of Jupiter on December 7, 1995. Measurements of the chemical and isotopic composition of the Jovian atmosphere were obtained by the mass spectrometer during the descent over the 0.5 to 21 bar pressure region over a time period of approximately 1 hour. The sampling was either of atmospheric gases directly introduced into the ion source of the mass spectrometer through capillary leaks or of gas, which had been chemically processed to enhance the sensitivity of the measurement to trace species or noble gases. The analysis of this data set continues to be refined based on supporting laboratory studies on an engineering unit. The mixing ratios of the major constituents of the atmosphere hydrogen and helium have been determined as well as mixing ratios or upper limits for several less abundant species including: methane, water, ammonia, ethane, ethylene, propane, hydrogen sulfide, neon, argon, krypton, and xenon. Analysis also suggests the presence of trace levels of other 3 and 4 carbon hydrocarbons, or carbon and nitrogen containing species, phosphine, hydrogen chloride, and of benzene. The data set also allows upper limits to be set for many species of interest which were not detected. Isotope ratios were measured for 3He/4He, D/H, 13C/12C, 20Ne/22Ne, 38Ar/36Ar and for isotopes of both Kr and Xe.     

Spatial heterogeneity in the radiogenic activity of the lunar interior: Inferences from CHACE and LLRI on Chandrayaan-1

In the past, clues on the potential radiogenic activity of the lunar interior have been obtained from the isotopic composition of noble gases like Argon. Excess Argon (40) relative to Argon (36), as compared to the solar wind composition, is generally ascribed to the radiogenic activity of the lunar interior. Almost all the previous estimates were based on, ‘on-the-spot’ measurements from the landing sites. Relative concentration of the isotopes of ⁴⁰Ar and ³⁶Ar along a meridian by the Chandra’s Altitudinal Composition Explorer (CHACE) experiment, on the Moon Impact Probe (MIP) of India’s first mission to Moon, has independently yielded clues on the possible spatial heterogeneity in the radiogenic activity of the lunar interior in addition to providing indicative ‘antiquity’ of the lunar surface along the ground track over the near side of the moon. These results are shown to broadly corroborate the independent topography measurements by the Lunar Laser Ranging Instrument (LLRI) in the main orbiter Chandrayaan-1. The unique combination of these experiments provided high spatial resolution data while indicating the possible close linkages between the lunar interior and the lunar ambience.     

The chemical conditions on the parent body of the murchison meteorite: Some conclusions based on amino, hydroxy and dicarboxylic acids

Amino and hydroxy acids have been identified in the Murchison meteorite. Their presence is consistent with a synthetic pathway involving aldehydes, hydrogen cyanide and ammonia in an aqueous environment (Strecker-cyanohydrin synthesis). From the various equilibrium and rate constants involved in this synthesis, four independent estimates of the ammonium ion concentrations on the parent body at the time of compound synthesis are obtained; all values are about 2 × 10^?3 M. Succinic acid and β-alanine have also been detected in the Murchison meteorite. Their presence is consistent with a synthesis from acrylonitrile, hydrogen cyanide and ammonia. Using the equilibrium and rate constants for this synthetic pathway, and the succinic acid/β-alanine ratio measured in the Murchison meteorite, an estimate of the hydrogen cyanide concentration of 10^?3 to 10^?2 M is obtained. Since hydrogen cyanide hydrolyzes relatively rapidly in an aqueous environment ($\text{t}{}_{\mathrm{<mtext>1</mtext><mtext>2</mtext>}}\text{< 10}{}^4\text{yrs}$) this high concentration implies a period of synthesis of organic compounds as short as 10⁴ years on the Murchison meteorite parent body.     

The Kumtag meteorite strewn field

The Kumtag meteorite strewn field was found in the Kumtag desert, 132 km south of Hami city in the Xinjiang province, China. It is an ellipse of 2.5 × 7.9 km, with a long axis extending along the northeast-southwest direction. The largest individual meteorite of the strewn field weighs about 10 kg; the smallest individual has a mass of only 27 g. In total, more than 100 individuals with a total mass of more than 180 kg were collected. The location and the distribution of the fragments suggest that the Kumtag meteoroid entered the atmosphere in the direction Northeast-Southwest. All meteorites collected in this strewn field are samples from the same unique meteorite shower. The Kumtag meteorite is an H5 ordinary chondrite with a shock stage S2, and a weathering grade W2. The cosmic ray exposure age of Kumtag is 6.7 ± 0.8 Ma, which is rather typical for H chondrites and which indicates that Kumtag was derived from the massive impact event on its parent body ~7 Ma ago. A significant amount of He has been lost during certain unknown processe(s) before the Kumtag meteorite was ejected from its parent body.     

Characteristics and formation of amino acids and hydroxy acids of the Murchison meteorite.

Eight characteristics of the unique suite of amino acids and hydroxy acids found in the Murchison meteorite can be recognized on the basis of detailed molecular and isotopic analyses. The marked structural correspondence between the alpha-amino acids and alpha-hydroxy acids and the high deuterium/hydrogen ratio argue persuasively for their formation by aqueous phase Strecker reactions in the meteorite parent body from presolar, i.e., interstellar, aldehydes, ketones, ammonia, and hydrogen cyanide. The characteristics of the meteoritic suite of amino acids and hydroxy acids are briefly enumerated and discussed with regard to their consonance with this interstellar-parent body formation hypothesis. The hypothesis has interesting implications for the organic composition of both the primitive parent body and the presolar nebula.     

Origin of organic compounds in carbonaceous chondrites.

Carbonaceous chondrites, a class of primitive meteorite, have long been known to contain their complement of carbon largely in the form of organic, i.e., hydrocarbon-related, matter. Both discrete organic compounds and an insoluble, macromolecular material are present. Several characteristics of these materials provide evidence for their abiotic origin. The principal formation hypotheses have invoked chemistry occurring either in the solar nebula or on the parent body. However, recent stable isotope analyses of the meteorite carboxylic acids and amino acids indicate that they may be related to interstellar cloud compounds. These results suggest a formation scheme in which interstellar compounds were incorporated into the parent body and subsequently converted to the present suite of meteorite organics by the hydrothermal process believed to have formed the clay minerals of the meteorite matrix.