宁强碳质球粒陨石基质及暗色边化学成份研究

采用仪器中子活化方法分析了宁强碳质球粒陨石基质及暗色边化学成份。结果表明,宁强陨石的基质比全岩富集轻稀土和亲硫元素,并大致具有与Allende陨石基质相似的稀土特征。暗色边与陨石基质的差别在于:前者富FeO而贫难熔元素。推测陨石基质与暗色边物质来源于太阳星云不同区域。与形成暗色边有关的突发性事件可能曾多次在太阳星云的不同区域中发生。     

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.     

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．     

我国九个球粒陨石化学组成的研究

在球粒陨石化学组成的研究中,经过试验我们建立了测定各化学元素的分析流程,测定了九个球粒陨石样品中各元素的含量,根据测定结果论证了它们各自所属的化学群、氧化还原趋势以及某些共同特征。     

亳县陨石中球粒的主量和微量元素的丰度特征及其启示

用仪器中子活化法分析了毫县(LL3-4)陨石中14个球粒的Al,Mg,Mn,Na,V,La,Sm,Au,Sc,Cr,Fe,Co,Ni,Eu,Ir等元素的含量。该陨石的球粒平均成分对Mg和Cl球粒陨石标准化值与其它不平衡普通球粒陨石一致。通过模糊聚类分析和因子分析讨论了元素间的相关关系。这些球粒的原始物质组分至少包括亲铁元素,难熔和中等难熔亲石元素以及中等挥发性元素等,这也与其它不平衡普通球粒陨石大体一致。因此,普通球粒陨石各化学群的差别主要是由基质造成的。      

清镇陨石（EH3）中陨硫钙石的REE微量元素及成因意义

本文运用INAA分析了14个清镇陨石中陨硫钙石单矿物颗粒的难熔元素(La、Ce、Sm、Eu、Yb、Lu、Ca、Sc、Hf和Th),挥发性元素(Na、Cr、Zn、Se、Br等)和亲铁元素(Fe、Ni、Co、Ir、Au、As)含量。结果表明陨硫钙石高度富集难熔亲石元素,是顽火辉石陨石中REE的主要载体,携带了约80％的全岩REE总量。相对于HREE,LREE有更大的富集程度,而且早期凝聚的颗粒较晚期凝聚的颗粒更富集REE,同时陨硫钙石富集挥发性元素Se、Br等。清镇陨硫钙石的微量元素特征揭示了它来自于太阳星云的高温凝聚特征和成因。     

清镇顽火辉石球粒陨石（EH3）的反射光谱特征

本文测定了清镇高铁群3型非平衡顽火辉石球粒陨石(EH3)的可见和近红外反射光谱,发现其反射光谱既不同于显示Ni、Fe金属光谱特征的EH4(Abee)顽火辉石球粒陨石,也不同于显示陨硫铁光谱特征的EH5型和EL6型平衡顽火辉石球粒陨石.清镇陨石独特的反射光谱特征可能是由于其铁纹石粒子表面存在光学厚度的吸积薄膜.吸积薄膜物质很可能是与铁纹石密切共生的陨硅磷镍铁矿,也可能是它与硫化矿物的混合物.在清镇陨石中,含吸积薄膜的铁纹石粒子可能具有很低的氧逸度,它们极易被大气氧化而失去原有的反射光谱特征.文中讨论了EH3、EH4、EH5和EL6型顽火辉石球粒陨石具有不同反射光谱特征的宇宙化学机理.     

铁陨石中若干元素的仪器中子活化分析及其化学分类

本文采用堆中子和超硼中子活化方法对Mundrabilla、浙江宁波、湖北黄陵、河北商都、广西南丹、贵州董岭、四川乐山、广西邕宁、新疆准噶尔等九个铁陨石和吉林陨石的金属颗粒作了分析,测定了Ge,Ga,Ir,Ni,Au,As,Cu和Co等八个元素的含量。并对九个铁陨石作了化学群的分类,它们分别属于ⅠAB,ⅢAB,ⅢCD和IVA群。南丹和董岭铁陨石的化学组成极为相似,它们可能是“成对”的铁陨石。      

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。      

H型球粒陨石TL灵敏度与冲击相和钾含量的研究

测定了坠落在我国武安、枣阳、信阳等地的10个H型球粒陨石的热释光(TL)灵敏度、自然热释光峰温和峰半高宽温度,同时对它们的K含量进行了测定.将测得的H型球粒陨石的TL灵敏度与它们的钾含量和所属冲击相进行比较.结果表明,H型球粒陨石的TL灵敏度与其钾含量和冲击相之间存在着规律性的关系.      

球粒陨石中单球粒硅含量测定及其意义

本工作采用14MeV中子活化分析方法,测定了20个单球粒及全岩的硅含量.结果表明:E、H、L、LL群石陨石中单球的硅含量均高于全岩的硅含量;全岩硅含量,按E、H、L、LL的次序,有逐步增高的趋势;非磁性单球硅含量,在普通球粒陨石中,按H、L、LL次序逐步增高.单球中硅含量高于全岩,间接证明凝聚形成球粒稍早于基质.      

Cometary constraints on the planet forming environment.

Molecular elemental and isotopic abundances of comets provide sensitive diagnostics for models of the primitive solar nebula. New measurements of the N2, NH and NH2 abundances in comets together with the in situ Giotto mass spectrometer and dust analyzer data provide new constraints for models of the comet forming environment in the solar nebula. An inventory of nitrogen-containing species in comet Halley indicates that NH3 and CN are the dominant N carriers observed in the coma gas. The elemental nitrogen abundance in the gas component of the coma is found to be depleted by a factor approximately 75 relative to the solar photosphere. Combined with the Giotto dust analyzer results for the coma dust component, we find for comet Halley Ngas + dust approximately 1/6 the solar value. The measurement of the CN carbon isotope ratio from the bulk coma gas and dust in comet Halley indicates a significantly lower value, 12C/13C = 65 +/- 9 than the solar system value of 89 +/- 2. Because the dominant CN carrier species in comets remains unidentified, it is not yet possible to attribute the low isotope ratio predominantly to the bulk gas or dust components. The large chemical and isotopic inhomogeneities discovered in the Halley dust particles on 1 mu scales are indicative of preserved circumstellar grains which survived processing in the interstellar clouds, and may be related to the presolar silicon carbide, diamond and graphite grains recently discovered in carbonaceous chondrites. Less than 0.1% of the bulk mass in the primitive meteorites studied consists of these cosmically important grains. A larger mass fraction (approximately 5%) of chemically heterogeneous organic grains is found in the nucleus of comet Halley. The isotopic anomalies discovered in the PUMA 1 Giotto data in comet Halley are probably also attributable to preserved circumstellar grains. Thus the extent of grain processing in the interstellar environment is much less than predicted by interstellar grain models, and a significant fraction of comet nuclei (approximately 5%) may be in the form of preserved circumstellar matter. Comet nuclei probably formed in much more benign environments than primitive meteorites.     

Fluorescent organic matter in carbonaceous chondrites.

Fluorescent organic matter in carbonaceous chondrites was investigated using a microscope equipped with a fluorescence spectrophotometer. Fluorescent particles were observed in powdered CM2 carbonaceous chondrites (Y-74662, Y-7791198, and Murchison) without carbon enrichment by acid treatments. Although it was difficult to find fluorescent particles in powdered sample of C3 chondrites (ALH-77307, Y-791717, and Allende) without acid treatments, many fluorescent particles were observed after carbon enrichment by acid treatments. Fluorescence of coronene and shock-altered graphite were observed using the same microscope and the same conditions as those for carbonaceous chondrites.     

Complex organics in meteorites.

Complex macromolecular organic matter is present in carbonaceous chondrites as the most abundant organic matter and may be present in interstellar dusts and comets. With this view, our studies of the complex organic matter isolated from six CM2 chondrites, namely Yamato-74662, Yamato-791198, Yamato-793321, Yamato-86720, Belgica-7904, and Murchison are introduced and discussed in the text. The complex organic matter is acid-insoluble and organic solvent-insoluble, and therefore, it was examined by heating experiments to obtain information on its chemical constituents and characteristics. Three chondrites, Yamato-74662, Yamato-791198, and Murchison which have solvent-extractable organic compounds, such as amino acids, carboxylic acid, hydrocarbons, etc. possess thermally labile organic fraction in the complex organic matter. Organic compounds detected in the pyrolyzate of the complex organic matter number over 130 of which aromatic hydrocarbons are dominant. They appeared around 300 degrees C, and disappeared at about 600 degrees C with a maximum at 400-500 degrees C during the heating. On the other hand, the other three chondrites do not have the extractable organic compounds nor a thermally labile organic fraction. The presence or absence of the fraction in the complex organic matter likely indicates the presence or absence of the solvent-extractable organic compounds and relates to thermal history of the chondrite.     

Structure of high-molecular carbonaceous compound in carbonaceous chondrites and formation of IR-spectroscopically similar compounds in the laboratory.

Main components of carbonaceous matter in carbonaceous chondrites are high molecular organic matter. Examinations of the compounds using pyrolysis GC/MS and FT-IR indicated the structural resemblance of major part of the molecule for all of the compounds from different types of carbonaceous chondrites (8 Antarctic and 2 none-Antarctic meteorites). A carbonaceous matter derived from graphite on a shock experiment using a rail gun (1g projectile at 7 km/s) showed similar IR spectrum to those of the meteoritic high-molecular organic matter. C-60 fullerene also gave a similar compound (with minor differences in IR spectra) on a shock experiment under the same conditions. A shock experiment using coronene also examined.     

Amino acids in meteorites.

Carbonaceous chondrites carry a record of chemical evolution that is unparalleled among presently accessible natural materials. Within the complex suite of organic compounds that characterize these meteorites, amino acids occur at a total concentration that may reach 0.6 micromole g-1 meteorite (approximately 60 ppm). Both free amino acids and acid-labile amino acid derivatives have been found in hot-water extracts of a CI1 and seven CM2 chondrites. Although the amino acid composition of all CM2 chondrites is not the same, differences may be largely explicable on the basis of spontaneous and biologically-caused decomposition occurring during their terrestrial residence. The amino acids of the Murchison meteorite (CM2) have been extensively analyzed and 52 amino acids have been positively identified. Thirty three of these amino acids are unknown in natural materials other than carbonaceous chondrites. Thus the Murchison meteorite has recently been the major source of new naturally-occurring amino acids. The Murchison amino acids comprise a mixture of C2 through C8 cyclic and acyclic monoamino alkanoic and alkandioic acids of nearly complete structural diversity. Within the acyclic monoamino alkanoic acid series, primary alpha-amino alpha-branched amino acids are predominant. The concentrations of individual amino acids decline exponentially with increasing carbon number within homologous series. Amino acid enantiomers are found in approximately equal amounts. Eight of the terrestrial protein amino acids have been found.     

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。      

Fluxes and nuclear abundances of cosmic rays inside the magnetosphere using a transmission function approach

At 1 AU and outside the Earth’s magnetosphere, the relative abundances to protons for He (He/p), C (C/p) and Fe (Fe/p) nuclei were calculated using the observation data of AMS-01 (for p and He) and HEAO-3 (for C and Fe) above 0.8 GeV/nucleon. In addition, the transmission function (TF) for the GCR propagation inside the magnetosphere was evaluated using the IGRF and T96 (introduced by Tsyganenko and Stern) models to obtain permitted and forbidden trajectories inside the magnetosphere. The TF allowed one to derive the primary He-nuclei fluxes in the same geomagnetic regions of AMS-01 observations. These fluxes were found in good agreement with the observation data. Furthermore inside the magnetosphere in addition to the flux of helium, it allowed one to obtain those of the primary p, C, and Fe nuclei and the relative abundances of He, C and Fe nuclei to protons from the same observation data of AMS-01 and HEAO-3 above ≈0.8 GeV/nucleon. Up to a geomagnetic latitude of ≈45.84°, the relative isotopic abundances were found to depend on the mass number I_isot and, on average, range from a factor ≈2.31 up to ≈3.35 larger than those outside the magnetosphere at 1 AU. Thus, the magnetospheric isotopic/nuclear relative abundances differ from those inside the solar cavity and those in the interstellar space. The usage of the TF approach can allow one to determine the nuclear abundances in the magnetosphere at any geomagnetic latitude and, thus, any orbit, provided that the CR spectra are determined at 1 AU.