符山石玉的初步研究

近期在云南和广州市场上出现了一种玉石,与翡翠混合镶嵌,其外观与翡翠极为相似,对检测工作造成了复杂性。通过采用常规宝石学测试、岩矿鉴定和IR与XRD分析,对该玉石成品和原料样品的特征进行了研究。结果表明,该玉石的主要矿物组成为符山石,含少量的钙铝榴石,为一种符山石玉,其产地不详。根据该玉石的常规宝石学特征、偏光显微镜下的特征以及IR和XRD特征可明显地与翡翠相区分。     

中国的磷铁锂矿—磷锰锂矿系列矿物

磷铁锂矿与磷锰锂矿是一完全类质同象系列中两个端员矿物。磷锰锂矿在我国新疆伟晶岩中已有大量发现。笔者于1984年在福建南平稀有金属花岗伟晶岩中发现了典型的磷铁锂矿。此外,早在1980年笔者还在新疆青河富铍伟晶岩中发现了成分介于该类质同象系列中间的磷锰铁锂矿。对后两个产状的矿物进行了较详细的矿物化学成分和物理性质研究。结合前人的资料,文中系统地讨论了国内所发现的六个产状的磷铁锂矿-磷锰锂矿系列矿物的化学成分特征及变化规律,化学成分与光学性质、物理性质、晶胞参数等之间的相互关系,并系统地引用了大量国外资料作对比。讨论了矿物中Mg、Ca等含量对这些特征的影响。另外,笔者还研究了该系列矿物成分与红外光谱之间的关系,指出矿物的红外吸收谱带频率与铁锰比值间呈良好的线性关系,并给出了相关关系式。     

用氢氧化物共沉淀法研究热液体系REE（Nb,Ti）2O6型矿物的形成机理

作者进行了稀土铌钛氢氧化物共沉淀实验,对共沉淀物及其高温灼烧产物进行了XRD、IR、DTA和Raman研究,结合前人高温高压实验结果以及野外地质事实,提出了热液体系复杂氧化物矿物易解石和黑稀金矿的络合物高温水解、氢氧化物共沉淀、脱水去羟、聚合成核和结晶的成因模式。     

马鞍山绿松石中水的振动光谱表征及其意义

在室温和变温条件下对安徽马鞍山绿松石中水的结构特征进行红外吸收光谱和激光拉曼光谱分析研究,结果表明:绿松石中部分水分子与Cu2 结合成[Cu(H2O)4]2 水合离子,并在很大程度上制约了绿松石的颜色;马鞍山地区绿松石中结晶水的脱失温度约为303℃～310℃,结构水的脱失温度约为346℃～375℃。绿松石中H2O,OH-的振动是导致其水的激光拉曼光谱形成的主要原因,ν(OH)振动导致的强拉曼特征谱峰在3470 cm-1,3502 cm-1～3505 cm-1之间的弱谱峰则隶属3470 cm-1的次级谱峰,ν(H2O)的拉曼谱峰主峰位于3442 cm-1～3449 cm-1处。由ν(MFe,Cu-H2O)伸缩振动致平缓的拉曼谱峰主要分布在3074 cm-1～3303 cm-1附近。     

Implications of the Sample Rate on Large Space Telescopes

The frequency at which a large space telescope's (e.g. JWST's) detector chips are read, or the sample rate, is tightly coupled to many hardware and operational aspects of the telescope's instrument and data handling elements. In this paper we discuss many of the drivers and important implications of the sample rate: the data rate to the ground; onboard computer storage, bandwidth, and speed; the number of A→D chips, and therefore the overall size and power requirements of the analog electronics; cryocabling requirements; and detector noise and power. We discuss and parametrize these and other elements related to sample rate. Finally, we discuss the implications of sample rate in the context of achieving the most important science goals under the constraint of limited cost. This revised version was published online in July 2006 with corrections to the Cover Date.     

A NICMOS-3 based spectrograph for near infrared astronomy

We describe a design for a compact cooled spectrograph which incorporates two cameras and two collimators to achieve high throughput from 0.8 to 2.5m. The spectrograph utilizes multiple NICMOS 3 arrays, specially mounted to minimize their separation in the spectral dimension. This accommodates the broad wavelength range while providing extensive coverage in the spatial dimension.     

Infrared instruments for the Gemini 8-M telescopes

The Gemini Telescopes are being built to exploit the splendid infrared sites of Mauna Kea in Hawaii and Cerro Pachon in Chile. Both telescopes are being designed to deliver 0.1 arcsecond images at 2.2 m to the focal plane. This image size includes all tracking and enclosure effects. To exploit the superb infrared characteristics of the sites and telescopes we will require a new generation of IR instruments which will challenge both instrument designers and infrared array technologies.     

First experiences with ARNICA,the Arcetri observatory imaging camera

ARNICA (ARcetri Near Infrared CAmera) is the imaging camera for the near infrared bands between 1.0 and 2.5 m that Arcetri Observatory has designed and built as a common use instrument for the TIRGO telescope (1.5 m diameter, f/20) located at Gornergrat (Switzerland). The scale is 1 per pixel, with sky coverage of more than 4×4 on the NICMOS 3 (256×256 pixels, 40 m side) detector array. The optical path is compact enough to be enclosed in a25.4 cm diameter dewar; the working temperature of detector and optics is 76 K. We give an estimate of performance, in terms of sensitivity with an assigned observing time, along with some preliminary considerations on photometric accuracy.     

Cs+水合结构密度泛函理论计算研究

本文用密度泛函理论在WB97XD/gen def2-tzvp基组水平上对[Cs(H2O) n] +(n=1-15)水合团簇结构的振动光谱进行了研究。研究表明,随着水分子数的增加,在气相和液相中,8配位的Cs+ 水合团簇是最稳定的;随着水分子数的增加,Cs-O键长增大,Cs+上的电荷密度减小。当水分子数大于11时,Cs-O键长和Cs+上的电荷密度变化很小。O(H2O)-O(H2O)距离、∠O(H2O)-Cs-O(H2O)°统计结果表明,15个水分子足以形成Cs+的近似饱和水合层。此外,红外光谱显示[Cs(H2O)n]+水合团簇中O-H伸缩振动随着水分子数的增加而发生变化,由此可以作为鉴别水合层位置的一种参考方法。     

Unusual infrared fading of CH Cygni in 2006

Infrared observations of the unique symbiotic system CH Cyg in 2003–2006 are presented. Analysis of the observations has shown that a fairly dense dust structure (a cloud or a shell) appeared on the line of sight in August–November 2006. The dust grains in the new shell are similar in optical properties to graphite ones and their sizes are mostly within the range 0.14–0.16 μm. The dust shell is optically thick and its optical depth at 2.2 μm is τ(2.2) ≈ 0.97. The dust shell mass is M _d(06) ≈ 8 × 10⁻⁶ M _⊙ and the rate of matter flow into the shell has reached ∼2 × 10⁻⁵ M _⊙ yr⁻¹. Original Russian Text ? O.G. Taranova, V.I. Shenavrin, 2007, published in Pis’ma v Astronomicheskiĭ Zhurnal, 2007, Vol. 33, No. 8, pp. 598–603.