论当前我国北西部铀矿勘查关键技术

本文提出当前我国北西部铀矿勘查两项关键技术──中国北西部寻找大型超大型可地浸砂岩铀矿勘查技术和找矿勘探过程中地浸可行性评价技术，并论述了技术内容和技术开发目标。两项关键技术的开发研究和落实对扩大我国铀矿资源有现实意义。     

综合物探技术在小盘岭公路隧道选线中的应用

利用综合物探技术,查明岩体风化情况、围岩分类以及构造带分布,进而为公路隧道的选线提供足够的信息,具有重要的意义。采用先进的电阻率成像技术和高分辨率浅层地震勘探方法,在小盘岭公路选线时,取得了很好的应用效果。     

新建蒲虹公路过湿路基的换填施工技术研究

基于浦虹公路区域地质、构造、降雨和工程特征的分析,针对不同特点的过湿路段施用不同的换填方案.并相应地制定施工工艺、工艺流程和操作要点.实际工程表明.该换填施工技术符合相应的设计和规范要求,效果良好.     

生物膜过滤深度净化水技术研究

以古交镇城底煤矿生活污水处理厂二级出水为研究对象,采用F/BF净化工艺,进行了污水深度处理的生产性试验。研究表明,该工艺对二级处理后的生活污水具有稳定、高效的净化能力,出水水质基本达到地面水Ⅳ类标准,可用于工业冷却水和低压水暖锅炉补充水,具有显著的经济效益和环境效益。试验还对不同滤料进行了分析,认为作为工业废料的炉渣是一种廉价、高效的新型生物膜过滤材料。     

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)     

电离层延时对低轨卫星频率传递的影响分析

利用低轨卫星,对受干扰区域的卫星导航接收机进行频率传递,是提升其性能的一种有效手段.而电离层延时误差是影响传递效果的重要因素.对基于低轨卫星的频率传递应用背景进行了介绍,分析了其基本原理,并着重分析了电离层延时的存在对频率传递的影响,提出利用站间差历元差的方法对电离层延时进行修正.最后,通过仿真对理论分析进行了验证.结果表明,通过站间差历元差的手段,对当前电离层变化值进行求解与预测,可以将电离层延时误差的变化控制在一定范围,满足频率传递的要求.     

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.     

Smear fitting: a new image-deconvolution method for interferometric data

A new technique is presented for producing images from interferometric data. The method, 'smear fitting', makes the constraints necessary for interferometric imaging double as a model, with uncertainties, of the sky brightness distribution. It does this by modelling the sky with a set of functions and then convolving each component with its own elliptical Gaussian to account for the uncertainty in its shape and location that arises from noise. This yields much sharper resolution than clean for significantly detected features, without sacrificing any sensitivity. Using appropriate functional forms for the components provides both a scientifically interesting model and imaging constraints that tend to be better than those used by traditional deconvolution methods. This allows it to avoid the most serious problems that limit the imaging quality of those methods. Comparisons of smear fitting to clean and maximum entropy are given, using both real and simulated observations. It is also shown that the famous Rayleigh criterion (resolution = wavelength/baseline) is inappropriate for interferometers as it does not consider the reliability of the measurements.     

Study of Star/Galaxy Classification Based on the XGBoost Algorithm

Machine learning has achieved great success in many areas today. The lifting algorithm has a strong ability to adapt to various scenarios with a high accuracy, and has played a great role in many fields. But in astronomy, the application of lifting algorithms is still rare. In response to the low classification accuracy of the dark star/galaxy source set in the Sloan Digital Sky Survey (SDSS), a new research result of machine learning, eXtreme Gradient Boosting (XGBoost), has been introduced. The complete photometric data set is obtained from the SDSS-DR7, and divided into a bright source set and a dark source set according to the star magnitude. Firstly, the ten-fold cross-validation method is used for the bright source set and the dark source set respectively, and the XGBoost algorithm is used to establish the star/galaxy classification model. Then, the grid search and other methods are used to adjust the XGBoost parameters. Finally, based on the galaxy classification accuracy and other indicators, the classification results are analyzed, by comparing with the models of function tree (FT), Adaptive boosting (Adaboost), Random Forest (RF), Gradient Boosting Decision Tree (GBDT), Stacked Denoising AutoEncoders (SDAE), and Deep Belief Nets (DBN). The experimental results show that, the XGBoost improves the classification accuracy of galaxies in the dark source classification by nearly 10% as compared to the function tree algorithm, and improves the classification accuracy of sources with the darkest magnitudes in the dark source set by nearly 5% as compared to the function tree algorithm. Compared with other traditional machine learning algorithms and deep neural networks, the XGBoost also has different degrees of improvement.     

菲律宾蛤仔碱性磷酸酶的分离纯化及部分性质研究

经Tris-HCl缓冲液浸提、硫酸铵分级沉淀盐析、DEAE-Sepharose Fast Flow离子交换层析和Sephadex G-75凝胶过滤层析等步骤,从菲律宾蛤仔内脏团中分离得到碱性磷酸酶,SDS-PAGE显示为单一条带,提纯倍数为14.42,比活力达到131.08U/mg。酶学性质研究表明:该酶亚基分子量约44kD,最适反应温度为45℃,最适pH值为9.0,米氏常数Km为0.098mmol/L,最大反应速度Vmax为1.01μmol/(mL·min)。Ca2+、Mg2+对酶活力表现出显著的激活作用。