中国鲎基因组微卫星富集文库的构建及分析

本研究旨在从DNA分子水平上研究中国鲎(Tachypleus tridentatus)种群遗传多样性及种群结构等相关信息,以期为保护其野生群体种质资源提供科学依据。本研究通过生物素—磁珠富集法筛选微卫星标记,构建中国鲎基因组微卫星文库。基因组DNA经Fast Digest Tru1I酶切后,选取400 bp~1000 bp片段,用生物素标记的(GT)15、(CT)15混合探针与其杂交,杂交复合物与链霉亲和素磁珠结合,捕获含有重复序列的微卫星片段,纯化后连接PMD19-T载体克隆,构建基因组微卫星文库。从334个阳性克隆中随机选取196个片段大于400 bp的阳性克隆进行测序,共获得127个微卫星序列,其中完美型占69.3%、非完美型占11.0%、复合型占19.7%。除探针使用的GT和CT的重复序列外,还筛选到多碱基GCT、TGG、AAAC、ACAA、GATTT、TTTTA的重复序列。根据微卫星序列设计选择合成40对引物,结果显示其中3对具有较高多态性,可作为进一步评价中国鲎野生种质资源等遗传信息的有效遗传标记。     

国外自发地理信息研究进展及对我国的启示

在内涵解析的基础上,主要从数据质量评估、贡献者分类与动机以及法律议题三方面归纳与梳理国外自发地理信息的研究情况。相比较而言,我国对自发地理信息的研究无论从深度还是广度上都处于起步阶段,未来研究应从四个方面深入开展:政府主导下的公众贡献自发地理信息;数据质量控制;移动自发地理信息以及自发地理信息涉及的法律议题。     

基于珞珈一号与DMSP/OLS数据的辽宁省城市空间扩张分析

基于珞珈一号和DMSP/OLS夜间灯光数据,提取辽宁省城市空间用地信息并监测分析了2003—2018年城市空间扩张特征。结果表明:1)利用辽宁省DMSP/OLS长时间序列夜间灯光数据提出了一种适合校正长时间序列DMSP/OLS数据的校正方法,提高了数据的连续性和可对比性;2)弥补了统计数据在空间属性的不足,消除了过去单纯依靠统计数据分析城市空间扩张的弊端,为其他省市分析城市扩张提供新的遥感监测分析方法;3)在2003—2018年间,辽宁省城市空间扩张存在城市空间扩张与南方省份相比发展比较缓慢及协调性欠佳等问题。     

利用众源地理数据快速测制大比例尺军事地形图

针对特战实训演练中大比例尺军事地形图数据不足、现势性较差的问题,从特战用图需求出发,基于众源地理数据提出了一种快速、高效、经济、准确的大比例尺军事地形图测制方法。首先,介绍了众源地理数据的概念和特点,研究了众源地理数据的来源和获取方法。然后,在顾及军事地形图与民用地形图之间制图表达的差异后,设计了利用众源地理数据绘制大比例尺军事地形图的工艺流程。最后,基于ArcMap,绘制了某地1∶1万军事地形图并进行实验验证和精度分析。实验结果表明,该方法既可有效提高作业效率,又能满足成图精度要求,可为军事教学训练、指挥员用图决策提供重要参考。     

Chemical spots on the surface of the strongly magnetic Herbig Ae star HD 101412

Due to the knowledge of the rotation period and the presence of a rather strong surface magnetic field, the sharp‐lined young Herbig Ae star HD 101412 with a rotation period of 42 d has become one of the most well‐studied targets among the Herbig Ae stars. High‐resolution HARPS polarimetric spectra of HD 101412 were recently obtained on seven different epochs. Our study of the spectral variability over the part of the rotation cycle covered by HARPS observations reveals that the line profiles of the elements Mg, Si, Ca, Ti, Cr, Mn, Fe, and Sr are clearly variable while He exhibits variability that is opposite to the behaviour of the other elements studied. Since classical Ap stars usually show a relationship between the magnetic field geometry and the distribution of element spots, we used in our magnetic field measurements different line samples belonging to the three elements with the most numerous spectral lines, Ti, Cr, and Fe. Over the time interval covered by the available spectra, the longitudinal magnetic field changes sign from negative to positive polarity. The distribution of field values obtained using Ti, Cr, and Fe lines is, however, completely different compared to the magnetic field values determined in previous low‐resolution FORS 2 measurements, where hydrogen Balmer lines are the main contributors to the magnetic field measurements, indicating the presence of concentration of the studied iron‐peak elements in the region of the magnetic equator. Further, we discuss the potential role of contamination by the surrounding warm circumstellar matter in the appearance of Zeeman features obtained using Ti lines. (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

热带风压场平衡特征及其对GRAPES系统中同化预报的影响研究I:平衡特征分析

本文基于GRAPES全球模式的短期预报误差样本,利用赤道波动正规模态研究了热带风、压场平衡特征,并根据这些特征分析了线性平衡方程(LBE)在该区域应用时存在的问题。结果表明:(1)赤道波动能成功解释热带短期预报误差样本的大部分分量,对流层中层为60%~80%,对流层顶和平流层低层为80%以上。(2)在可解释的误差方差中,赤道罗斯贝波(ER)占比仅为30%~55%,其他赤道波动的作用不可忽视。(3)在ER模态基础上引入其他赤道波动会大幅削弱原有风、压场平衡约束,重力惯性波与Kelvin波的作用最为显著。此时,对流层中层位势高度h与u风、v风间的约束接近于零,而平流层低层h-u的平衡特征由Kelvin波主导。(4)LBE主要表达了ER模态下的风、压场平衡特征,与实际情形相比高估了热带风、压场的耦合程度,进一步的改进中需削弱这一虚假平衡,使得热带风、压场分析变得更加独立。     

Evaluation of radar and automatic weather station data assimilation for a heavy rainfall event in southern China

To improve the accuracy of short-term(0–12 h) forecasts of severe weather in southern China, a real-time storm-scale forecasting system, the Hourly Assimilation and Prediction System(HAPS), has been implemented in Shenzhen, China. The forecasting system is characterized by combining the Advanced Research Weather Research and Forecasting(WRF-ARW)model and the Advanced Regional Prediction System(ARPS) three-dimensional variational data assimilation(3DVAR) package. It is capable of assimilating radar reflectivity and radial velocity data from multiple Doppler radars as well as surface automatic weather station(AWS) data. Experiments are designed to evaluate the impacts of data assimilation on quantitative precipitation forecasting(QPF) by studying a heavy rainfall event in southern China. The forecasts from these experiments are verified against radar, surface, and precipitation observations. Comparison of echo structure and accumulated precipitation suggests that radar data assimilation is useful in improving the short-term forecast by capturing the location and orientation of the band of accumulated rainfall. The assimilation of radar data improves the short-term precipitation forecast skill by up to9 hours by producing more convection. The slight but generally positive impact that surface AWS data has on the forecast of near-surface variables can last up to 6–9 hours. The assimilation of AWS observations alone has some benefit for improving the Fractions Skill Score(FSS) and bias scores; when radar data are assimilated, the additional AWS data may increase the degree of rainfall overprediction.     

Finding the most variable stars in the Orion Belt with the All Sky Automated Survey

We look for high‐amplitude variable young stars in the open clusters and associations of the Orion Belt. We use public data from the ASAS‐3 Photometric V ‐band Catalogue of the All Sky Automated Survey, infrared photometry from the 2MASS and IRAS catalogues, proper motions, and the Aladin sky atlas to obtain a list of the most variable stars in a survey area of side 5° centred on the bright star Alnilam (ε Ori) in the centre of the Orion Belt. We identify 32 highly variable stars, of which 16 had not been reported to vary before. They are mostly variable young stars and candidates (16) and background giants (8), but there are also field cataclysmic variables, contact binaries, and eclipsing binary candidates. Of the young stars, which typically are active Herbig Ae/Be and T Tauri stars with Hα emission and infrared flux excess, we discover four new variables and confirm the variability status of another two. Some of them belong to the well known σ Orionis cluster. Besides, six of the eight giants are new variables, and three are new periodic variables (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Associations of decimetric type Ⅲ bursts with coronal mass ejections and Hα flares

We present a statistical study of decimetric type Ⅲ radio bursts,coronal mass ejections(CMEs),and Hα flares observed in the period from July 2000 to March2005.In total,we investigated 395 decimetric type Ⅲ radio burst events,21% of which showed apparent correlation to CMEs that were associated with Hα flares.We noticed that the Hα flares which were strongly associated with CMEs were gradual events,and82% of them took place before CMEs appeared in the field of view of LASCO C2;that most of the CME-associated radio bursts started in the frequency range around750 MHz with a frequency drifting rate of several hundred MHz s-1,of which both positive and negative ones were recognized; and that the correlation of type Ⅲ radio bursts to CMEs without associated flares is fairly vague,less than 9%.     

Pixel-based correction for Charge Transfer Inefficiency in the Hubble Space Telescope Advanced Camera for Surveys

Charge Transfer Inefficiency (CTI) due to radiation damage above the Earth's atmosphere creates spurious trailing in Hubble Space Telescope ( HST ) images. Radiation damage also creates unrelated warm pixels – but these happen to be perfect for measuring CTI. We model CTI in the Advanced Camera for Surveys (ACS)/Wide Field Channel and construct a physically motivated correction scheme. This operates on raw data, rather than secondary science products, by returning individual electrons to pixels from which they were unintentionally dragged during readout. We apply our correction to images from the HST Cosmic Evolution Survey (COSMOS), successfully reducing the CTI trails by a factor of ∼30 everywhere in the CCD and at all flux levels. We quantify changes in galaxy photometry, astrometry and shape. The remarkable 97 per cent level of correction is more than sufficient to enable a (forthcoming) reanalysis of downstream science products and the collection of larger surveys.