壳聚糖和PDMDAAC改性膨润土用于处理含油废水的研究

含油废水污染范围广,对人类和生态环境危害大。采用常规方法(如浮选法、絮凝法、电化学法、膜分离法和生物法)处理的除油率不高于91%,成本较高,因此急需开发一种高效低廉的吸附剂。膨润土是一种优良的吸附剂,但用其直接处理含油废水的效果较低。本文选用壳聚糖和PDMDAAC两种有机物作为改性剂,对钠基膨润土改性,使膨润土能有效地处理含油废水。通过实验比较了两种有机改性膨润土处理含油废水的最佳去除条件,探讨了表征对其吸附性能的影响。去油效果结果表明:壳聚糖改性膨润土的除油率可达87.8%,PDMDAAC改性膨润土的除油率可达89.3%,处理所需时间少于15 min;除油效率和处理时间都优于常规方法。吸附性能表征结果显示,两种改性剂均以负载的方式和钠基膨润土颗粒结合,吸附性能良好;相比而言,PDMDAAC改性膨润土的处理效果比壳聚糖改性膨润土更好。PDMDAAC应用于含油废水的处理,具有成本低、效率高、操作简单的特点,在含油废水处理领域具有较好的应用前景。     

断层失稳错动热场前兆模式：雁列断层的实验研究

在实验室使用红外热像仪和接触式测温仪同步观测记录了压性和张性雁列断层失稳错动前后的热场变化过程.从实验记录中发现，在断层失稳引起温度场和热红外辐射亮温温度场上升之前，在两断层段之间的岩桥区发生降温变化.断层带开始升温发生在失稳前2～3 s内，岩桥区的降温却发生在失稳前约20s，这两个超前时间长度相差近一个量级.此类热场先降后升变化过程在雁列构造变形中有一定的普遍性，可能作为雁列断层失稳错动的热场前兆模式.根据实验观测结果，详细描述了上述热场变化的时间过程及其空间分布特征，分析了产生此种失稳前兆模式的机制，显著异常出现的条件及有利观测部位，讨论了它在地震前兆探索等研究中的意义.     

应用ATOVS资料反演大气温湿廓线

本文用牛顿迭代的方法反演NOAA-15极轨气象卫星ATOVS资料，求解大气温度廓线和水汽廓线，本文利用一阶变分原理从辐射传输方程中得到了大气温度、水汽权重函数的解析形式，并改进了传统使用的线性迭代方法，利用牛顿非线性迭代方法求解大气表层温度，大气温度廓线及大气水汽廓线，并根据大气参量的自相关性，将大气温度廓线、大气水汽廓线用经验正交函数（EOF）的线性组合表示，减少了要反演的参数，提高了反演稳定性和迭代速度。     

An infrared and <Superscript>1</Superscript>H MAS NMR investigation of strong hydrogen bonding in ussingite,Na<Subscript>2</Subscript>AlSi<Subscript>3</Subscript>O<Subscript>8</Subscript>(OH)

The mineral ussingite, Na₂AlSi₃O₈(OH), an interrupted tectosilicate, has strong hydrogen bonding between OH and the other nonbridging oxygen atom in the structure. Infrared spectra contain a strongly polarized, very broad OH-stretching band with an ill-defined maximum between 1500 and 1800 cm^–1, and a possible OH librational bending mode at 1295 cm^–1. The IR spectra confirm the orientation of the OH vector within the triclinic unit cell as determined from X-ray refinement (Rossi et al. 1974). There are three distinct bands in the ¹H NMR spectrum of ussingite: a predominant band at 13.5 ppm (TMS) representing 90% of the structural hydrogen, a second band at 15.9 ppm corresponding to 8% of the protons, and a third band at 11.0 ppm accounting for the remaining 2% of structural hydrogen. From the correlation between hydrogen bond length and ¹H NMR chemical shift (Sternberg and Brunner 1994), the predominant hydrogen bond length (H...O) was calculated to be 1.49 Å, in comparison to the hydrogen bond length determined from X-ray refinement (1.54 Å). The population of protons at 15.9 ppm is consistent with 5–8% Al–Si disorder. Although the ussingite crystal structure and composition are similar to those of low albite, the bonding environment of OH in low albite and other feldspars, as characterized through IR and ¹H NMR, is fundamentally different from the strong hydrogen bonding found in ussingite.     

X射线荧光光谱法分析不同类型岩石中10种主量元素的测试能力验证

以28个不同类型岩石标样作外标,用玻璃熔片法制样,采用经验系数法进行基体校正,建立了X射线荧光光谱法(XRF)测定不同类型岩石中硅铝钙镁等10种主量元素的分析方法。该方法被用于参与GeoPT分析测试能力验证,15年来分析了23个不同类型的岩石验证样品。经验证该方法对SiO_2、Al_2O_3、K_2O和CaO具有非常好的分析效果(所有测定结果的|Z|2);对于MgO、MnO、TiO_2和Na_2O四个元素,尽管各有一个样品的分析结果的|Z|2,这主要是样品与标样的基体差异较大造成了低含量样品测定结果超差,但依然可获得好的分析效果;当TFe_2O_31.0%,P_2O_5含量在0.08%~0.80%区间时,分析结果的|Z|2,满足分析期望。总体上所建立的XRF分析方法稳定,可满足应用地球化学实验室测试不同类型岩石中10种主量元素的分析期望。     

Near-infrared imaging of H2 in molecular outflows from young stars

In an attempt to identify the molecular shocks associated with the entrainment of ambient gas by collimated stellar winds from young stars, we have imaged a number of known molecular outflows in H₂ v=1-0 S(1) and wide-band K. In each flow, the observed H₂ features are closely associated with peaks in the CO outflow maps. We therefore suggest that the H₂ results from shocks associated with the acceleration or entrainment of ambient, molecular gas. This molecular material may be accelerated either in a bow shock at the head of the flow, or along the length of the flow through a turbulent mixing layer.     

Infrared speckle imaging: Data reduction with application to binary stars

The extended Knox-Thompson reduction scheme currently in use at Kitt Peak National Observatory and Steward Observatory for the reduction of infrared speckle interferometry is described in detail. Applications of this algorithm and the less computationally intensive shift-and-add analysis to both simulated and real binary star data is presented demonstrating that the latter may be successfully used for image reconstruction by using a separately measured point source. The performance of both techniques is shown to improve by application of an iterative deconvolution algorithm to apply a priori image constraints without degradation of photometric information.Operated by the Association of Universities for Research in Astronomy Inc. (AURA) under cooperative agreement with the National Science Foundation     

Condensed species in Titan's stratosphere: Confirmation of crystalline cyanoacetylene (HC3N) and evidence for crystalline acetylene (C2H2) on Titan

Infrared spectra of crystalline HC₃N and C₂H₂ were investigated at several temperatures between 15 and 150 K. The characteristics of the 505 and 753 cm⁻¹ bands of HC₃N are in complete agreement with the emission spectral data on Titan obtained by the Voyager IRIS instrument, thus confirming the identification of crystalline HC₃N on Titan. A composite spectrum in the 720-800 cm⁻¹ region, with contributions from HC₃N and C₂H₂ in crystalline phases, reproduces the Voyager emission data in that region, thus providing a suggestion for the identification of crystalline C₂H₂ on Titan.     

Recent progress in imaging polarimetry

Recent instrumental developments in imaging polarimetry allow array detectors to reach a polarimetric sensitivity of 1 × 10^–4 of the intensity. New instrumental effects appear at these levels of sensitivity and generate spurious polarization signals with amplitudes of up to 5 × 10^–4. Here I discuss these effects and present methods to avoid them. Polarized spectra with an rms noise of 6 × 10^–6 may then be obtained. Furthermore a method is brought to the reader's attention that allows polarization measurements at the 1 × 10^–4 level with regular array detectors, e.g. in the near-infrared.