红土镍矿样品前处理方法和分析测定技术研究进展

随着常规镍来源的硫化镍矿资源的日益枯竭,可直接生产氧化镍、镍锍和镍铁等产品的红土镍矿倍受关注。对于红土镍矿中主量、次量、痕量元素的检测,相同的检测项目存在多种测试方法,且部分相同原理的测试方法存在细节上的差异,使得检测者选择合适的检测方法变得困难。本文综述了近年来红土镍矿中24种元素测定的样品前处理方式及分析技术研究进展。样品前处理方式依据目标元素及后续的分析方法进行选择,其中酸溶法和碱熔法用途最广。酸溶法引入的盐分少,操作简单,但是分解过程中易导致挥发元素As、Sb、Bi、Hg的损失,Cr易随高氯酸冒烟损失。碱熔法分解能力强,适合分析Cr、Si、全铁等项目,但会引入大量的盐类和因坩埚材料损耗而带入其他杂质,给后续分析带来困难。红土镍矿的分析技术依据实验室条件及目标元素的性质和浓度进行选择。电感耦合等离子体发射光谱法(ICP-AES)是主量、次量元素的主要分析方法,适合于分析含量为10-5~30%级别的金属元素;X射线荧光光谱法主要用于分析含量为10-3~1级别的元素,尤其适合于测定Al、Si、Ti、V和P,由于该方法的准确性依赖于一套高质量的标准样品,故更适合炉前检测或检测大批红土镍矿样品。电感耦合等离子体质谱法(ICP-MS)最适合于分析10-4含量以下的重元素,特别是稀土和贵金属元素。原子吸收光谱法(AAS)适合于分析10-4~10-2级别的Ca、Mg、Ni、Co、Zn、Cr、Mn等低沸点、易原子化元素。分光光度法主要用于分析Ni和P。原子荧光光谱法(AFS)主要用于分析As、Bi、Sb等易形成气态氢化物的元素。容量法主要用于分析Al、Fe、Mg和Si O2等主含量元素。尽管AAS、分光光度法、AFS法和容量法检测周期长,但所用仪器为实验室常规配置,可满足缺乏相应大型仪器实验室的日常检测。本文认为,针对各种检测方法的适用性及存在问题,应从开发微波消解法、固体进样直接测汞法、ICP-MS法以及Cr与其他元素同时分析的快速分析方法等方面开展研究,建立灵敏、准确的检测方法,从而更好地服务于红土镍矿的贸易、检验和综合利用。     

空间分析技术在研究传染病时空传播规律中的应用

以手足口病为例,介绍了地理信息的空间统计技术在传染病时空传播规律研究中的应用,包括传染病空间分布模式研究、传染病聚集性分析、传染病扩散传播模式分析、传染病发病率空间自相关分析及传染病发病率空间回归模型预测方面的研究,为传染病防治决策提供科学依据,具有一定的实用性。     

TanDEM-X双站SAR干涉测量及研究进展

较全面、系统地介绍了Tan DEM-X/Terra SAR-X双站SAR科学计划,重点涉及其科学目标、Tan DEM-X卫星参数、轨道结构以及干涉数据获取模式等相关内容,并讨论了双站SAR成像、极化In SAR和数字波束成形等干涉测量新技术及其研究进展。这些双站SAR新技术的实现将大大地推动SAR干涉测量在全球地形测绘、冰川学、海洋学及地质学等领域中的应用。     

Digitization of sunspot drawings by Spörer made in 1861–1894

Most of our knowledge about the Sun's activity cycle arises from sunspot observations over the last centuries since telescopes have been used for astronomy. The German astronomer Gustav Spörer observed almost daily the Sun from 1861 until the beginning of 1894 and assembled a 33‐year collection of sunspot data covering a total of 445 solar rotation periods. These sunspot drawings were carefully placed on an equidistant grid of heliographic longitude and latitude for each rotation period, which were then copied to copper plates for a lithographic reproduction of the drawings in astronomical journals. In this article, we describe in detail the process of capturing these data as digital images, correcting for various effects of the aging print materials, and preparing the data for contemporary scientific analysis based on advanced image processing techniques. With the processed data we create a butterfly diagram aggregating sunspot areas, and we present methods to measure the size of sunspots (umbra and penumbra) and to determine tilt angles of active regions. A probability density function of the sunspot area is computed, which conforms to contemporary data after rescaling. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

New spectroscopic and polarimetric observations of the A0 supergiant HD 92207

Our recent search for the presence of a magnetic field in the bright early A‐type supergiant HD 92207 using FORS 2 in spectropolarimetric mode revealed the presence of a longitudinal magnetic field of the order of a few hundred Gauss. However, the definite confirmation of the magnetic nature of this object remained pending due to the detection of shortterm spectral variability probably affecting the position of line profiles in left‐ and right‐hand polarized spectra. We present new magnetic field measurements of HD 92207 obtained on three different epochs in 2013 and 2014 using FORS 2 in spectropolarimetric mode. A 3σ detection of the mean longitudinal magnetic field using the entire spectrum, 〈B_z〉_all = 104 ± 34 G, was achieved in observations obtained in 2014 January. At this epoch, the position of the spectral lines appeared stable. Our analysis of spectral line shapes recorded in opposite circularly polarized light, i.e. in light with opposite sense of rotation, reveals that line profiles in the light polarized in a certain direction appear slightly split. The mechanism causing such a behaviour in the circularly polarized light is currently unknown. Trying to settle the issue of short‐term variability, we searched for changes in the spectral line profiles on a time scale of 8–10 min using HARPS polarimetric spectra and on a time scale of 3–4 min using time series obtained with the CORALIE spectrograph. No significant variability was detected on these time scales during the epochs studied. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Variable stars in the Bochum Galactic Disk Survey

We present a first overview of variable stars in the Bochum Galactic Disk Survey (GDS) with emphasis on eclipsing binaries (EBs). This ongoing survey is performed by a robotic twin refractor at the Universitätssternwarte Bochum located near Cerro Armazones in Chile. It comprises a mosaic of 268 fields in a stripe of Δb = ±3° along the Galactic plane observed once per month simultaneously in the Sloan r and i filters with a detection limit of r_s ∼ 16 mag and i_s ∼ 15 mag. The data from the first three years until the end of February 2014 yields a total of 41718 variable stars with variability amplitudes between 0.1–6 mag. A cross‐match with SIMBAD identified 11 465 of these variables unambiguously, while 2184 had multiple matches; most of the remaining stars could be matched with 2MASS objects. Among the SIMBAD‐listed objects with single matches, only 1982 turned out as known variables while a further 256 are suspected of variability. That leaves a total of 39480 potentially new variables. The group of known variables comprises 419 stars (21 %) that are classified as EBs while 443 (22%) are of other types; for the remaining 1120 catalogued variables (57 %) the type is unknown. Investigating variability as a function of spectral type, we find that SIMBAD provides spectral types for 2811 (25 %) of the identified stars. Spectral classes B (26 %), A (20 %), and M (25%) contain the most numerous variables, while all other classes contribute less than 10% each. More than half of the B (55 %) and A (56%) stars are designated as EBs, suggesting that hundreds of new B‐ and A‐type EBs may be contained in the GDS archive. In contrast, among the numerous M stars no EBs are known. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Discovery of a new blue quasar: SDSS J022218.03–062511.1

We report the discovery of a bright blue quasar: SDSS J022218.03–062511.1. This object was discovered spectroscopically while searching for hot white dwarfs that may be used as calibration sources for large sky surveys such as the Dark Energy Survey or the Large Synoptic Survey Telescope project. We present the calibrated spectrum, spectral line shifts and report a redshift of z = 0.521±0.0015 and a rest‐frame g‐band luminosity of 8.71×10¹¹ L_⊙. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

A Preliminary Research on the Development of the Hard X-ray Imaging Telescope

The hard X-ray imaging telescope based on the Fourier transform imaging technique is introduced. The double-layer parallel gratings are used to make the modulation and coding on the light emerging from a celestial X-ray source, the modulated light is acquired, to make the optoelectronic conversion by scintillation crystal detectors, and ?nally read out by the electronic system. The modulation collimator X-ray telescopes can be divided into two types: the spatial modulation and temporal modulation. The temporal modulation system requires the scanning motion of the detector system, but the spatial modulation system requires no motion. The technology of grating fabrication is investigated, and the basic structure design of the collimators is given. The principal compo- nents of the prototype hard X-ray imaging telescope of spatial modulation type are successfully developed, including the 8 CsI crystal detector modules (contain- ing photomultipliers or PMTs), 8-channel shaping ampli?ers (two of them are prepared for experiments), and the data acquisition system. And the preliminary test results of the electronic system are also given.