埃塞俄比亚染色欧泊的研究

目前,埃塞俄比亚染色欧泊在我国市场上屡见不鲜.本文采用常规宝石学测试手段、光谱分析、吸水实验、浸泡褪色实验和浸泡染色实验等方法对市场上常见的3种颜色的埃塞俄比亚染色欧泊进行了研究.结果表明,这些埃塞俄比亚染色欧泊主要通过浸泡于不同颜色的化学颜料溶液中上色,浸泡过程中往往添加含有羧酸根离子的表面活性剂或颜料超分散剂(如邻苯二甲酸酯),以使颜料颗粒分布更加均匀,这主要是由于埃塞俄比亚欧泊的孔隙度相对较大,对染料的吸附性相对较强.这些埃塞俄比亚染色欧泊的主要特征如下: ① 亚透明至微透明,染橙色和染蓝色样品具有弱至强的变彩,染黑色样品体色以灰蓝色或黄灰色为主,具有强烈的红色、黄色、绿色和蓝色变彩;透射光下照射,染黑色欧泊具有强至弱的红色调以及明显的染剂不均匀富集现象. ② 埃塞俄比亚染色欧泊和其天然欧泊一样吸水性强,吸水后密度、质量均有所增加,透明度增强,变彩可能会有所增强,也可能会有所减弱,染色欧泊密度范围为1.63～1.86 g/cm³,折射率在1.40(点测)左右,与天然欧泊一致,均低于澳大利亚和墨西哥的欧泊. ③ 在高倍显微镜下观察,染色样品颜色分布不均,内部常见色点、色斑、色块或色团分布,在表面部位染剂富集现象更为明显,常见染剂沿着边缘、刮痕或凹坑处富集. ④ 染色欧泊浸泡在不同的溶剂中会使溶剂变色. ⑤ 拉曼光谱表明,染色欧泊出现了很强的荧光背景及弱的热效应峰3 362 cm^-1,拉曼散射峰很弱. ⑥ 紫外可见光分光光谱表明,埃塞俄比亚染色欧泊与天然欧泊的吸收光谱不同.     

基于粘滞性声波方程的吸收补偿方法

通常地层介质都是粘滞性的,由于地层的吸收作用,地震波在向下传播过程中能量被衰减,特别是高频能量的衰减,使反射信号频带宽度变窄。为了补偿被吸收的能量,笔者采用粘滞声波方程波场延拓方法进行能量吸收和衰减补偿。首先,从粘滞性波动方程波场延拓函数理论出发,推导了波场延拓函数稳定性条件;其次,对其有效性进行了测试和分析;最后,通过设计数值模型进行正演模拟对比试验,证明了基于粘滞性声波方程的吸收补偿方法能够很好地对粘性介质吸收衰减进行能量补偿,改善处理效果。     

Adsorption behaviors of Cd^2＋ on Fe2O3/MnO2 and the effects of coexisting ions under alkaline conditions

This study describes the adsorption features of cadmium on Fe2O3 and MnO2 in alkaline saline conditions. The adsorption reached equilibrium in 6 hours under alkaline conditions. The absorption of cadmium on Fe2O3 and MnO2 was consistent with Freundlich absorption isotherms, and the corresponding adsorption capacities were 16.3 and 16.7 mg·g-1, respectively. Moreover, the adsorption quantity of cadmium on Fe2O3 and MnO2 rose with increasing pH from acidic to neutral, and reached the maximum at pH= 9. The coexisting chlorides reduced the adsorption capacity of Fe2O3 and MnO2. The influence intensities of different cations follow the order of CaCl2>>KCl>NaCl. However, the influence of sodium salts on the capacities of Fe2O3 and MnO2 to adsorb cadmium appeared more complicated: the relatively low concentrations of sodium salts could reduce the adsorption capacity; with increasing concentrations of sodium salts, e.g. NaCl and NaNO3. The adsorption capacity decreased continually. Moreover, due to the competition adsorption and precipitation effects, the adsorption capabilities of Na2CO3, NaH2PO4 and Na2HSO4 could also be reduced and cadmium concentrations in the solution were reduced as well.     

微量石棉的X射线衍射定量检测

微量(质量分数低至0.1%)石棉的定量分析是一世界性难题。研究了自行车、电动车车闸等摩擦材料中石棉含量为0.1%~5.0%(质量分数)的X射线衍射定量分析方法。对含有微量石棉的样品通过X射线衍射的基底吸收修正法,求出定量分析试样中的石棉含量,计算出石棉的比例。研究成果对支持我国自行车、电动车等产品出口日本的工作具有现实意义。     

次灵敏线-火焰原子吸收光谱法连续测定 高品位矿石中的铜铅锌量

[摘要]分别以铜327郾4 nm 和249郾2nm、铅283郾3 nm 和261郾4nm、锌307郾6nm 次灵敏线为分析线, 火焰原子吸收光谱法测定了高品位矿石中铜、铅、锌的含量。考察了高品位矿石基体及主要杂质的干扰 情况,结果表明,铜、锌质量浓度小于2 mg/ ml 时,对铅的测定无干扰;铅质量浓度小于2 mg/ ml 时,对铜 测定无干扰,其质量浓度小于0郾5mg/ ml 时,对锌测定无干扰;测定溶液中主要杂质铁、钴、镍、钙、镁质量 浓度在1mg/ ml,铝、硅质量浓度在0郾2mg/ ml 对测定无干扰。铜铅锌的质量浓度分别在0 ~ 1000滋g/ ml 范围内呈良好的线性关系。方法的精密度(RSD,n=5) 小于5%,加标回收率在98郾91% ~ 101郾08%,测 定铜铅锌矿石国家标准物质,结果与标准值相符。     

X-ray Spectromicroscopy of Mineral Intergrowths in the Santa Catharina Meteorite

This work describes the application of microfocus X-ray absorption spectroscopy (XAS) and X-ray photo-emission electron microscopy (XPEEM) to the study of the complex mineralogical intergrowths within the Santa Catharina meteorite. The Santa Catharina meteorite of this study (BM52283 from the meteorite collection of the Natural History Museum, London, UK) primarily comprises a taenite bulk host phase (Fe:Ni ratio = 70.9 ± 0.8%:29.1 ± 0.8%) with a set of oxide-bearing cloudy zone textured regions (Fe:Ni:O ratio = 40.4 ± 0.3%:49.0 ± 0.7%:10.6 ± 0.8% at the core and Fe:Ni:O ratio = 34.4 ± 1.5%:42.7 ± 0.6%:22.9 ± 1.8% towards the rims) and numerous schreibersite (Fe:Ni:P ratio = 38.6 ± 1.6%:38.4 ± 0.9%:23.0 ± 0.5%) inclusions. Between the schreibersite and the taenite are rims up to 50 μm across of Ni-rich kamacite (Fe:Ni ratio = 93.4 ± 0.4%:6.6 ± 0.5%). No chemical zoning or spatial variations in the Fe and Ni speciation was observed within either the schreibersite or the kamacite phases. The oxide-bearing cloudy zone textured regions mostly comprise metallic Fe–Ni alloy, predominantly tetrataenite. Within the oxide phases, the Fe is predominantly, but not entirely, tetrahedrally co-ordinated Fe³⁺ and the Ni is octahedrally co-ordinated Ni²⁺. Structural analysis supports the suggestion that non-stoichiometric Fe₂NiO₄ trevorite is the oxide phase. The trevorite:tetrataenite ratio increases at the edges of the oxide-bearing cloudy zone textured regions indicating increased oxidation at the edges of these zones. The spatial resolution of the XPEEM achieved was between 110 and 150 nm, which precluded the study of either the previously reported ∼ 10 nm precipitates of tetrataenite within the bulk taenite or any antitaenite.     

水体富营养化状态对城市河道底泥吸附/释放P的影响 ——以江苏省苏州市河道试验研究为例

以苏州古城区内的河道为研究对象,采用静态培养的方式,研究了上覆水体不同富营养化程度对底泥中P释放/吸附的影响。研究结果表明：截断外源污染后,苏州河道底泥对水体中营养盐P呈现吸收状态;随着上覆水体磷酸盐浓度的增大,单位面积底泥累积吸收的磷酸盐就越多;上覆水与底泥比值越大,底泥对P的吸附率有减小的趋势。     

On variations in the fine-structure constant and stellar pollution of quasar absorption systems

At redshifts   z _abs≲ 2  , quasar absorption-line constraints on space–time variations in the fine-structure constant, α, rely on the comparison of Mg  ii and Fe  ii transition wavelengths. One potentially important uncertainty is the relative abundance of Mg isotopes in the absorbers, which, if different from solar, can cause spurious shifts in the measured wavelengths and, therefore, α. Here we explore chemical evolution models with enhanced populations of intermediate-mass (IM) stars, which, in their asymptotic giant branch phase, are thought to be the dominant factories for heavy Mg isotopes at the low metallicities typical of quasar absorption systems. By design, these models partially explain recent Keck/HIRES evidence for a smaller α in   z _abs < 2  absorption clouds than on Earth. However, such models also overproduce N, violating observed abundance trends in high- z _abs damped Lyman-α (DLA) systems. Our results do not support the recent claim of Ashenfelter et al. that similar models of IM-enhanced initial mass functions (IMFs) may simultaneously explain the HIRES varying-α data and DLA N abundances. We explore the effect of the IM-enhanced model on Si, Al and P abundances, finding it to be much less pronounced than for N. We also show that the ¹³C/¹²C ratio, as measured in absorption systems, could constitute a future diagnostic of non-standard models of the high-redshift IMF.     

Tracing the warm–hot intergalactic medium in the local Universe

We present a simple method for tracing the spatial distribution and predicting the physical properties of the Warm–Hot Intergalactic Medium (WHIM), from the map of galaxy light in the Local Universe. Under the assumption that biasing is local and monotonic we map the  ∼2 h ⁻¹ Mpc  smoothed density field of galaxy light into the mass-density field, from which we infer the spatial distribution of the WHIM in the Local Supercluster. Taking into account the scatter in the WHIM density–temperature and density–metallicity relation, extracted from the z = 0 outputs of high-resolution and large-box-size hydrodynamical cosmological simulations, we are able to quantify the probability of detecting WHIM signatures in the form of absorption features in the X-ray spectra, along arbitrary directions in the sky. To illustrate the usefulness of this semi-analytical method we focus on the WHIM properties in the Virgo cluster region.     

Physical effects on the Lyα forest flux power spectrum: damping wings, ionizing radiation fluctuations and galactic winds

We explore several physical effects on the power spectrum of the Lyα forest transmitted flux. The effects we investigate here are not usually part of hydrodynamic simulations and so need to be estimated separately. The most important effect is that of high column density absorbers with damping wings, which add power on large scales. We compute their effect using the observational constraints on their abundance as a function of column density. Ignoring their effect leads to an underestimation of the slope of the linear theory power spectrum. The second effect we investigate is that of fluctuations in the ionizing radiation field. For this purpose we use a very large high-resolution N -body simulation, which allows us to simulate both the fluctuations in the ionizing radiation and the small-scale Lyα forest within the same simulation. We find an enhancement of power on large scales for quasars and a suppression for galaxies. The strength of the effect rapidly increases with increasing redshift, allowing it to be uniquely identified in cases where it is significant. We develop templates that can be used to search for this effect as a function of quasar lifetime, quasar luminosity function and attenuation length. Finally, we explore the effects of galactic winds using hydrodynamic simulations. We find the wind effects on the Lyα forest power spectrum to be degenerate with parameters related to the temperature of the gas that are already marginalized over in cosmological fits. While more work is needed to conclusively exclude all possible systematic errors, our results suggest that, in the context of data analysis procedures, where parameters of the Lyα forest model are properly marginalized over, the flux power spectrum is a reliable tracer of cosmological information.