Simulations of self-magnetization in dusty space plasmas comparing different charge polarities and charge numbers of the dust

In partially ionized dusty space plasmas collisional momentum transfer between neutral and charged components of different inertia yields significant self-induced magnetic fields on remarkable short time scales of several dust Alfven times. Considering the proto-solar accretion disk previous first self-consistent plasma-neutral gas-dust simulations have shown, that this process yields a self-magnetization of 10^-5- on time scales of about 100 days. Thus, this mechanism is able to explain the remanent magnetization of chondrite type meteorite matter. New simulations show the quantitative dependence of the self-magnetization on polarity and charge numbers of the dust grains.     

Origin of Halogens and Nitrogen in Enstatite Chondrites

The EH and EL enstatite chondrites are the most reduced chondrite groups, having formed in nebular regions where the gas may have had high C/O and/or pH₂/pH₂O ratios. Enstatite chondrites (particularly EH) have higher CI- and Mg-normalized abundances of halogens (especially F and Cl) and nitrogen than ordinary chondrites and most groups of carbonaceous chondrites. Even relative to CI chondrites, EH and EL chondrites are enriched in F. We have found that literature values for the halogen abundance ratios in EH and EL chondrites are strongly correlated with the electronegativities of the individual halogens. We suggest that the most reactive halogens were the most efficient at forming compounds (e.g., halides) that were incorporated into EH-chondrite precursor materials. It seems plausible that, under the more-oxidizing conditions pertaining to the other chondrite groups, a larger fraction of the halogens remained in the gas. Nitrogen may have been incorporated into the enstatite chondrites as simple nitrides that did not condense under the more-oxidizing conditions in the regions where other chondrite groups formed. Literature data show that unequilibrated enstatite chondrites have light bulk N (δ ¹⁵N ≈ −20‰) compared to most ordinary (−5 to +20‰) and carbonaceous (+20 to +190‰) chondrites; this may reflect the contribution in enstatite chondrites of nitride condensates with δ¹⁵ N values close to the proposed nebular mean (~−400‰). In contrast, N in carbonaceous chondrites is mainly contained within ¹⁵N-rich organic matter. The major carrier of N in ordinary chondrites is unknown.     

南极格罗夫山陨石的磁化率

我国在南极格罗夫山发现并收集到大量南极陨石,需要一种无损、快速简单的分类方法。陨石磁化率(χ)的主要贡献是其中的铁镍金属,因而有可能成为一种简便有效的分类参数。同时,磁化率是陨石的一个重要物理参数。我们在国内首次开展陨石磁化率的研究,通过对模拟陨石磁化率样品的测量,证明可以通过不同取向的测量平均,将样品的大小和形状等几何因素的影响减小在仪器的测量精度范围之内。完成了首批613块南格格罗夫山陨石的磁化率测量,除普通球粒陨石外,还包括火星陨石、灶神星陨石、碳质球粒陨石、中铁陨石、橄榄陨铁、橄辉无球粒陨石等特殊类型。根据质量磁化率,可以划分大部分H、L、LL群陨石。特别重要的是,磁化率对于划分非平衡的普通球粒陨石化学群提供了更为可靠的参数。格罗夫山H群陨石的磁化率分布与南极其他地区的陨石十分相似,二者相对降落型陨石均向低质量磁化率方向平移0.2（logχ, 10^-9m³/kg）,反映了风化作用对南极陨石磁化率的平均影响程度;格罗夫山L群陨石的质量磁化率分布同样较降落型陨石偏低0.2左右,但南极其他地区的陨石与沙漠陨石的磁化率分布相似,二者均更为离散和偏低,可能反映了不同的风化程度。     

华南泥盆纪Chondrites的特征及其对古氧相的示踪

系统描述了发育于广西六景、贵州独山、贵阳乌当泥盆纪3个浅海沉积区Cruziana遗迹相Chondrites的产出特征,结合华南泥盆纪其他5个浅海沉积区Cruziana遗迹相的Chondrites资料,对Chondtites的寄主岩系颜色分级、遗迹组构、潜穴直径、遗迹属种的综合研究表明,只有寄主岩系为深灰色-黑色,岩性为灰岩、泥灰岩,潜穴直径小于1 mm,无其他遗迹化石共生时,Chondrites才是贫氧环境标志性遗迹化石的新认识,而个体粗大的Chondrites常发育在常氧环境中.     

Transport of solids in protoplanetary disks: Comparing meteorites and astrophysical models

We review models of chondrite component transport in the gaseous protoplanetary disk. Refractory inclusions were likely transported by turbulent diffusion and possible early disk expansion, and required low turbulence for their subsequent preservation in the disk, possibly in a dead zone. Chondrules were produced locally but did not necessarily accrete shortly after formation. Water may have been enhanced in the inner disk because of inward drift of solids from further out, but likely not by more than a factor of a few. Incomplete condensation in chondrites may be due to slow reaction kinetics during temperature decrease. While carbonaceous chondrite compositions might be reproduced in a “two-component” picture (Anders, 1964), such components would not correspond to simple petrographic constituents, although part of the refractory element fractionations in chondrites may be due to the inward drift of refractory inclusions. Overall, considerations of chondrite component transport alone favor an earlier formation for carbonaceous chondrites relative to their non-carbonaceous counterparts, but independent objections have yet to be resolved.     

The nature,origin and modification of insoluble organic matter in chondrites,the major source of Earth’s C and N

All chondrites accreted ∼3.5 wt.% C in their matrices, the bulk of which was in a macromolecular solvent and acid insoluble organic material (IOM). Similar material to IOM is found in interplanetary dust particles (IDPs) and comets. The IOM accounts for almost all of the C and N in chondrites, and a significant fraction of the H. Chondrites and, to a lesser extent, comets were probably the major sources of volatiles for the Earth and the other terrestrial planets. Hence, IOM was both the major source of Earth’s volatiles and a potential source of complex prebiotic molecules.Large enrichments in D and ¹⁵N, relative to the bulk solar isotopic compositions, suggest that IOM or its precursors formed in very cold, radiation-rich environments. Whether these environments were in the interstellar medium (ISM) or the outer Solar System is unresolved. Nevertheless, the elemental and isotopic compositions and functional group chemistry of IOM provide important clues to the origin(s) of organic matter in protoplanetary disks. IOM is modified relatively easily by thermal and aqueous processes, so that it can also be used to constrain the conditions in the solar nebula prior to chondrite accretion and the conditions in the chondrite parent bodies after accretion.Here we review what is known about the abundances, compositions and physical nature of IOM in the most primitive chondrites. We also discuss how the IOM has been modified by thermal metamorphism and aqueous alteration in the chondrite parent bodies, and how these changes may be used both as petrologic indicators of the intensity of parent body processing and as tools for classification. Finally, we critically assess the various proposed mechanisms for the formation of IOM in the ISM or Solar System.     

柴达木盆地南缘石炭系Chondrites遗迹化石的发现及其地质意义

在柴达木盆地南缘野外地质调查过程中,在祁曼塔格山前石拐子剖面下石炭统石拐子组和乌图美仁庆华铁矿附近剖面的上石炭统缔敖苏组中发现了大量Chondrites遗迹化石。经鉴定,研究区的Chondrites遗迹化石主要包括Chondrites fenxiangensis Yang,1984（分乡丛藻迹）;Chondrites filifalx Volk,1964（细枝丛藻迹）和Chondrites maqianensis Yang,1988（玛沁丛藻迹）3个遗迹种。根据研究区的Chondrites遗迹化石特征,结合岩性特征和其他实体化石资料,认为石拐子地区早石炭世为台洼沉积环境,乌图美仁庆华铁矿地区晚石炭世为局限碳酸盐岩台地沉积环境。另外,探讨了生物扰动对两个地区储集层的改造作用。该研究对恢复柴达木盆地南缘的沉积环境和古生态以及评价研究区的储集层物性具有重要的借鉴意义。     

湖北宜昌王家湾五峰组顶部Chondrites的发现及其环境意义

本文报道了湖北宜昌王家湾剖面五峰组笔石页岩段观音桥层发现的遗迹化石Chondrites的分布及其生态特点。结合生物相和同期上扬子海盆相对海平面的变化,分析了盆地水体底域在缺氧一富氧转折时期的古氧相变化特征：指出五峰组笔石页岩段上部地层沉积底域为典型的缺氧环境,在其与上覆观音桥段之间的沉积转换面附近发生了从无氧到有氧的转变,观音桥段中Hirnantia动物群繁盛于富氧的海底环境。     

A micro-Raman survey of 10 IDPs and 6 carbonaceous chondrites

This paper presents a micro-Raman survey of a set of 10 IDPs and 6 pristine carbonaceous chondrites. The higher sensitivity of the present micro-spectrometers allowed to record a dozen of spectra for each objects, whereas only one was available in previous studies. First, as in previous studies, the first-order carbon bands G and D were the only detected features, superimposed onto a fluorescence background of variable intensity, and the spectral characteristics of these bands point to a very disordered polyaromatic organic matter (OM). Nevertheless, these new data reveal that in IDPs, unlike chondrites, the presence of the Raman bands is not systematic, evidencing a much higher heterogeneity in the spatial distribution or the chemical composition of OM. Second, as a consequence, a single spectrum is not representative of a whole IDP, and the classification previously proposed by Wopenka [ 1988. Raman observations on individual interplanetary dust particules. Earth and Planet. Sci. Lett. 88, 221—231.] is no longer tenable. At last, this study shows that the fluorescence signal induced by the laser irradiation mostly originates from OM.