Tektite glass in apollo 12 sample

The glassy portion of lunar sample 12013 from Apollo 12 is chemically more like some tektites from Java than like any terrestrial igneous rock. It satisfies all the chemical criteria for a tektite. Tektites are relatively recent and acid rocks, whereas the moon is chiefly ancient and basaltic; hence, tektites are probably ejected volcanically, rather than by impact, from the moon.     

Mineralogy and petrology of coarse particulate material from lunar surface at tranquillity base

Five grams of coarse fines (10085,11) contains 1227 grains, mostly mafic holocrystalline rock fragments, microbreccia, and glass spatter and agglomerates with less abundant anorthosite fragments and regularly shaped glass. The crystalline lithic fragments in the coarse fines and microbreccias represent a closely related suite of gabbroid igneous rocks that have a wider range of modal analyses and textures than seen in the larger crystalline rock samples returned by Apollo 11. Petrographic evidence of shock metamorphism is common, and the abundant glass is almost all shock-produced. None of the glass observed is similar to tektite glass.     

Preliminary examination of lunar samples from apollo 14

The major findings of the preliminary examination of the lunar samples are as follows: 1) The samples from Fra Mauro base may be contrasted with those from Tranquillity base and the Ocean of Storms in that about half the Apollo 11 samples consist of basaltic rocks, and all but three Apollo 12 rocks are basaltic, whereas in the Apollo 14 samples only two rocks of the 33 rocks over 50 grams have basaltic textures. The samples from Fra Mauro base consist largely of fragmental rocks containing clasts of diverse lithologies and histories. Generally the rocks differ modally from earlier lunar samples in that they contain more plagioclase and contain orthopyroxene. 2) The Apollo 14 samples differ chemically from earlier lunar rocks and from their closest meteorite and terrestrial analogs. The lunar material closest in composition is the KREEP component (potassium, rare earth elements, phosphorus), "norite," "mottled gray fragments" (9) from the soil samples (in particular, sample 12033) from the Apollo 12 site, and the dark portion of rock 12013 (10). The Apollo 14 material is richer in titanium, iron, magnesium, and silicon than the Surveyor 7 material, the only lunar highlands material directly analyzed (11). The rocks also differ from the mare basalts, having much lower contents of iron, titanium, manganese, chromium, and scandium and higher contents of silicon, aluminum, zirconium, potassium, uranium, thorium, barium, rubidium, sodium, niobium, lithium, and lanthanum. The ratios of potassium to uranium are lower than those of terrestrial rocks and similar to those of earlier lunar samples. 3) The chemical composition of the soil closely resembles that of the fragmental rocks and the large basaltic rock (sample 14310) except that some elements (potassium, lanthanum, ytterbium, and barium) may be somewhat depleted in the soil with respect to the average rock composition. 4) Rocks display characteristic surface features of lunar material (impact microcraters, rounding) and shock effects similar to those observed in rocks and soil from the Apollo 11 and Apollo 12 missions. The rocks show no evidence of exposure to water, and their content of metallic iron suggests that they, like the Apollo 11 and Apollo 12 material, were formed and have remained in an environment with low oxygen activity. 5) The concentration of solar windimplanted material in the soil is large, as was the case for Apollo 11 and Apollo 12 soil. However, unlike previous fragmental rocks, Apollo 14 fragmental rocks possess solar wind contents ranging from approximately that of the soil to essentially zero, with most rocks investigated falling toward one extreme of this range. A positive correlation appears to exist between the solar wind components, carbon, and (20)Ne, of fragmental rocks and their friability (Fig. 12). 6) Carbon contents lie within the range of carbon contents for Apollo 11 and Apollo 12 samples. 7) Four fragmental rocks show surface exposure times (10 x 10(6) to 20 x 10(6) years) about an order of magnitude less than typical exposure times of Apollo 11 and Apollo 12 rocks. 8) A much broader range of soil mechanics properties was encountered at the Apollo 14 site than has been observed at the Apollo 11, Apollo 12, and Surveyor landing sites. At different points along the traverses of the Apollo 14 mission, lesser cohesion, coarser grain size, and greater resistance to penetration was found than at the Apollo 11 and Apollo 12 sites. These variations are indicative of a very complex, heterogeneous deposit. The soils are more poorly sorted, but the range of grain size is similar to those of the Apollo 11 and Apollo 12 soils. 9) No evidence of biological material has been found in the samples to date.     

A possible tektite strewn field in the Argentinian Pampa

Impact glass associated with 11 elongate depressions in the Pampean Plain of Argentina, north of the city of Rio Cuarto, was suggested to be proximal ejecta related to a highly oblique impact event. We have identified about 400 additional elongate features in the area that indicate an aeolian, rather than an impact, origin. We have also dated fragments of glass found at the Rio Cuarto depressions; the age is similar to that of glass recovered 800 kilometers to the southeast. This material may be tektite glass from an impact event around 0.48 million years ago, representing a new tektite strewn field.     

贵州遵义地区表层土壤微量元素均匀化现象及其农业地质环境效应

利用1：50000遵义市、遵义县2幅区域土壤地球化学调查成果，对该区土壤中环境微量元素分布特征及地球化学异常作了分析，认为岩石风化形成的土壤微量元素含量受控于母岩，但表层土壤长期经受相同的风化作用后，其土壤微量元素具有相似的特征，出现土壤微量元素总量均匀化现象，说明土壤中元素经过长期风化后，各元素在不同区域土壤中的含量基本相同，出现均匀化现象，依据这个特征可判断土壤的风化程度。     

Zircon and chromite crystals in a muong nong-type tektite

Chromite, zircon, and quartz crystals (identified by x-ray diffraction) have been recovered from a 2.07-gram sample of Muong Nong-type tektite. The absence of eskolaite (Cr(2)O(3)) and baddeleyite (ZrO(2)) supports a previous conclusion that Muong Nong-type tektites were not heated as intensely as other tektite groups. X-ray asterism studies indicate that the crystals are shocked, which supports an impact origin. The presence of chromite and zircon together suggests that the Muong Nong-type tektite was produced from sedimentary material.     

Lunar anorthosites: rare-Earth and other elemental abundances

Elemental abundances of major (Ti, Al, Fe, and Ca), minor (Na, Mn, and Cr), and trace elements [14 rare-earth elements (REE), Y, In, Cd, Rb, Cs, Ba, Co, and Sc] in lunar anorthosites separated from Apollo 11 sample 10085 coarse fines have been determined by means of instrumental and radiochemical neutron activation analysis. The REE distribution pattern of lunar anorthosites, relative to ordinary chondrites, has a positive Eu anomaly. On the assumption that (i) the lunar composition is similar to that of ordinary chondritic meteorites low in total Fe ( approximately 13 percent); (ii) lunar anorthosites are derived from highland cratering events and are representative of the highlands; and (iii) the moon differentiated into olivine, hypersthene, and basaltic and anorthositic phases, and plagioclase crysstallization began after approximately 93 percent solidification, then mass balance calculations yield approximately 30-kilometer and approximately 10-kilometer thicknesses for the lunar highlands for the melting and chemical differentiation of the entire moon and of the upper 200 kilometers, respectively. Corresponding thicknesses of the basaltic basement rocks were approximately 5 kilometers and approximately 2 kilometers, respectively. Alternatively, if the anorthosites of this study are representative of the highlands and the onset of plagioclase crystallization occurred after approximately 50 percent solidification of the initially melted moon, calculations with REE and Ba partition coefficients suggest that the REE and Ba abundances in the primeval moon were similar to those observed in basaltic achondrites.     

Argon-40/ argon-39 dating of lunar rock samples

Seven crystalline rock samples returned by Apollo 11 have been analyzed in detail by means of the (40)Ar-(-39)Ar dating technique. The extent of radiogenic argon loss in these samples ranges from 7 percent to >/= 48 percent. Potassium-argon ages, corrected for the effects of this loss, cluster relatively closely around the value of 3.7 x 10(9) years. Most of the vulcanism associated with the formation of the Mare Tranquillitatis presumably occurred around 3.7 x 10(9) years ago. A major cause of the escape of gas from lunar rock is probably the impact event which ejected the rock from its place of origin to its place of discovery. Upper limits for the times at which these impact events occurred have been estimated.     

马尾松凋落物分解过程中的微量元素释放动态

为探索马尾松(Pinus massonana)凋落物在不同密度林分中微量元素的释放规律,以12 a生马尾松人工林为研究对象,采用网袋分解法,分析3种密度下马尾松凋落物分解过程中干质量损失率、4种微量元素含量和养分残留率变化。结果表明,马尾松人工林凋落物残留率在不同密度间的变化趋势均相近,密度对残留率无显著影响。不同月份残留率不同,11月至翌年1月迅速降低,然后减缓,春季和夏季加快降低,秋季又开始减缓。凋落物中4种微量元素释放模式主要为"淋溶-富集-释放"(Zn除外)。经过1 a分解,各密度林分凋落物的干质量均损失过半;平均养分残留率从大到小为Cu(84.9%)、Fe(66.3%)、Mn(55.9%)、Zn(52.6%);凋落物中Zn残留率随密度增大而减小,其他养分变化不明显。     

黔西南铊成矿区微量元素地球化学特征研究

对采集于黔西南铊矿床(点)及其外围的31件矿物、矿石、蚀变围岩、未蚀变岩石进行了INAA分析。结果表明,样品中微量元素含量与玄武岩含量相差较大,与中酸性岩浆岩的含量非常相似,与在该地区地层中发现中酸性岩浆矿物相印证。     

Chemistry of rocks and soils in Gusev Crater from the alpha particle x-ray spectrometer

The alpha particle x-ray spectrometer on the Spirit rover determined major and minor elements of soils and rocks in Gusev crater in order to unravel the crustal evolution of planet Mars. The composition of soils is similar to those at previous landing sites, as a result of global mixing and distribution by dust storms. Rocks (fresh surfaces exposed by the rock abrasion tool) resemble volcanic rocks of primitive basaltic composition with low intrinsic potassium contents. High abundance of bromine (up to 170 parts per million) in rocks may indicate the alteration of surfaces formed during a past period of aqueous activity in Gusev crater.     

岩扇贝闭壳肌营养成分的分析及与中国3种扇贝的比较

为研究岩扇贝Crassadoma gigantea闭壳肌的营养成分,采用常规营养分析方法,对岩扇贝及虾夷扇贝Patiopecten yesoensis、海湾扇贝Argopecten irradians和栉孔扇贝Chlamys farreri闭壳肌的一般营养成分、氨基酸组成、脂肪酸组成、部分矿物元素含量进行了测定,并对4种扇贝闭壳肌营养成分进行了比较分析与评价。结果表明:岩扇贝闭壳肌中水分、粗蛋白质、粗脂肪、灰分和总糖的质量分数(鲜计)分别为78.68%、16.13%、0.92%、1.77%和1.92%,与另3种扇贝相比,岩扇贝闭壳肌的粗蛋白质与灰分含量相对较高,水分与粗脂肪含量较低,总糖含量与虾夷扇贝接近,高于栉孔扇贝,低于海湾扇贝;岩扇贝闭壳肌中必需氨基酸总量(EAA)为5.17%,占氨基酸总量的35.54%,必需氨基酸与非必需氨基酸的比为59.10%,略高于其他3种扇贝,接近FAO/WHO的理想氨基酸模式,呈味氨基酸(DAA)总量为7.25%,占氨基酸总量的49.82%;岩扇贝闭壳肌中高度不饱和脂肪酸(HUFA)含量占总脂肪酸的48.56%,其中EPA和DHA占总脂肪酸的41.84%,略高于海湾扇贝和栉孔扇贝;岩扇贝闭壳肌矿物元素中常量元素的含量依次为KMgCa,微量元素中Zn含量较为丰富。研究表明,岩扇贝闭壳肌具有高蛋白质、低脂肪的特点,食用价值和保健作用较高,是一种具有潜在引种价值的扇贝。     

Microtektites and tektites: a chemical comparison

Elemental abundance (20 trace elements, 3 major elements) comparisons for Ivory Coast microtektites and Australasian microtektites indicate that there are distinct chemical similarities between microtektites and nearby tektites. Several trace element abundances in microtektites are quite different from those observed in Apollo 11 and Apollo 12 samples.     

Emission spectrographic determination of trace elements in lunar samples

Eighteen minor or trace elelnents were detected and determined by emission spectroscopy. Direct d-c arc excitation of powdered samnples was used with three variations in the procedure. Thirteen lunar samples consisting of four finegrained igneous rocks, one medium-grained igneous rock, seven breccias, and one sample of fines were analyzed. The zinc and nickel concentrations in the breccias were approximately one order of magnitude greater than the concentrations of these elements in igneous rocks.     

Glazed lunar rocks: origin by impact

The glassy coating of lunar rock 12017 is enriched in 15 trace elements relative to the crystalline interior. It apparently consists chiefly of shock-melted rock, somewhat richer in rare earth elements and alkali metals than rock 12017 itself. The glass has been contaminated by about 0.5 percent carbonaceous-chondrite-like material or, alternatively, by a mixture of 0.06 to 0.3 percent fractionated meteoritic material and approximately 10 to 15 percent local soil. The glazing seems to represent molten material splashed from a nearby meteorite impact and not in situ melting by a sudden increase in solar luminosity.     

Magnetic properties of lunar dust and rock samples

Determinations on 20-to 80-milligram portions of the rock samples and the -150 mesh fraction of the lunar dust show pronounced Curie points between 680 degrees and 780 degrees C. Remanent intensities of five rock fragments vary from 8.4 x 10(-5) to 0.30 X J0(-5) emu/gram. Upon demagnetization, two of the samples had only viscous magnetization and two other samples had stable magnetizations with remanent coercivities in excess of 50 oersteds. Partial thermal demagnetization suggests that these apparently stable moments may have been acquired in a magnetic field in excess of 1500 gammas. xsxs.     

云南不同地区麻疯树种子微量元素分析

经HNO3-HClO4湿法消解样品,使用电感耦合等离子体原子发射光谱（ICP—OES）测定不同产地麻疯树种子中必需元素的含量。结果显示：Fe为35—134μg/g,Cu为26—37μg/g,Mn为15～41μg/g,Zn为54～126μg/g,Ca为5331～7428μg/g,Mg为9909～11817μg/g,K为12735～14503μg/g,P为17240～19239μg/g。其中Cu,Fe,Mn,Zn4种元素在各样品中含量差异显著。麻疯树种子中必需元素含量较为丰富。     

The proton microprobe: a powerful tool for nondestructive trace element analysis

A proton microprobe capable of focusing proton beams with energies up to 6 million electron volts to a spot size of 2 x 2 square micrometers has been used for chemical analysis of small grains of minerals in lunar samples by proton-induced x-ray emission. The proton microprobe is preferable to the electron microprobe for analyzing trace elements whose concentrations are below the detection limit of the latter and for analyzing objects with numerous major and trace elements with a wide range of atomic numbers. Application of the proton microprobe to biological samples is feasible.     

生物强化处理油田含油污泥的试验研究

采用油泥、菌剂及其他添加物充分混合后堆放的方法,进行了3种条件下的微生物对含油污泥的强化分解研究。结果表明,在菌剂和锯末的共同作用下,经过45d后,污泥含油量从24%下降到11%,去除率达到54%;而菌剂单独作用下,含油量下降到16%,去除率达为33%;在没有菌剂作用下,含油量仍然保持在20%以上。对处理过程中pH变化特性进行了研究。试验说明,生物强化分解是含油污泥处理的有效途径。     

Recent developments in the analysis of toxic elements

One may conclude that it is impractical to confine oneself to any one analytical method since ever more sensitive instrumentation continues to be produced. However, in certain methods such as anodic stripping voltammetry and flameless atomic absorption it may be background contamination from reagent impurities and surroundings rather than instrument sensitivity which controls the limits of element detection. The problem of contamination from dust or glassware is greatly magnified when the sample size becomes ever smaller. Air entering laboratories near highways may contain trace quantities of lead, cadmium, barium, antimony, and other elements from engine exhaust. Even plastic materials contacting the sample may be suspect as a source of contamination since specific metals may be used as catalysts in the synthesis of the plastic and traces may be retained in it. Certain elements may even be deliberately added to plastics during manufacture for identification purposes. Nondestructive methods such as neutron activation and x-ray techniques thus offer great advantages not only in time but in the elimination of impurities introduced during sample ashing. Future improvements in attainable limits of detection may arise largely from progress in the ultrapurification of reagents and "clean-room" techniques. Finally, the competence of the analyst is also vitally important in the skillful operation of modern complex analytical instrumentation and in the experienced evaluation of data.