伊利石单元粒子及其研究意义

单元粒子是单晶体构成的细小的粘土颗粒,是由一种或多种层状结构的硅酸盐构成的混层粘土的基本单元。多数伊利石单元粒子以混层晶体的"建筑砌块"的形式产出,"砌块"与"砌块"之间,在 a、b方向通过"砌块"的边缘界面相"砌合"而连接,在 c轴方向通过平面界面相"砌合"而连接。还对伊利石单元粒子的生长机理及形成过程中的形态变化、利用伊利石单元粒子的厚度划分成岩作用阶段等方面的研究成果进行了综述。伊利石单元粒子的形成过程有三个阶段：蒙脱石伊利石化过程中2nm厚的伊利石粒子的成核作用阶段、成核作用与生长作用阶段和表面控制生长阶段。伊利石单元粒子生长过程中,伊利石单元粒子呈现从板状体到条状体的生长,而板状颗粒又呈现各种螺旋生长图案,有圆形、残缺的圆形、多边螺旋、平行阶梯状螺旋、交错螺旋等。伊利石单元粒子的厚度分布服从对数正态型,其峰值为10.5nm。单元粒子与纳米科技两者的主要研究内容和所采用的方法基本一致,建议今后将研究单元粒子与研究纳米粘土矿物学有机地结合起来。     

卡尔曼滤波在VLBI数据处理中的应用

本文探讨卡尔曼滤波技术用于VLBI天体测量和大地测量数据处理的原理和方法;并深入地对Herring等提出的软件系统（SOLVK）进行详细研究,提出一些具体的办法以便应用．然后用1993—1994年的VLBI观测资料,精确计算了几种天文学和地球动力学参数作为例证．     

Extended source effects in astrometric gravitational microlensing

Extended source size effects have been detected in photometric monitoring of gravitational microlensing events. We study similar effects in the centroid motion of an extended source lensed by a point mass. We show that the centroid motion of a source with uniform surface brightness can be obtained analytically. For a source with a circularly symmetric limb-darkening profile, the centroid motion can be expressed as a one-dimensional integral, which can be evaluated numerically. We find that when the impact parameter is comparable to the source radius, the centroid motion is significantly modified by the finite source size. In particular, when the impact parameter is smaller than the source radius, the trajectories become clover-leaf like. Such astrometric motions can be detected using space interferometers such as the Space Interferometry Mission . Such measurements offer exciting possibilities for determining stellar parameters, such as stellar radius, to excellent accuracy.     

基于混沌时间序列的Volterra自适应滤波极移预报方法

针对极移复杂的时变特性, 根据混沌相空间坐标延迟重构理论, 提出一种基于Volterra自适应滤波的极移预报方法. 首先, 利用最小二乘拟合算法分离极移序列中的线性趋势项、钱德勒项和周年项, 获得线性极移、钱德勒极移和周年极移的外推值; 其次, 通过C-C关联积分法对最小二乘拟合残差序列进行相空间重构, 并利用小数据量法计算残差序列的最大Lyapunov指数验证其混沌特性, 在此基础上, 构建Volterra自适应滤波器对残差序列进行预测; 最后, 将线性极移、钱德勒极移和周年极移的外推值以及最小二乘拟合残差的预测值相加获得极移最终预报值. 利用国际地球自转服务局(International Earth Rotation and Reference Systems Service, IERS)提供的极移数据进行1--60d跨度预报, 并将预报结果分别与国际地球定向参数预报比较竞赛(Earth Orientation Parameters Prediction Comparison Campaign, EOP PCC)结果和IERS A公报发布的极移预报产品进行对比, 结果表明: 对于1--30d的短期预报, 该方法的预报精度与EOP PCC最优预报方法相当, 当预报跨度超过30d时, 该方法的预报精度低于EOP PCC最优预报方法, 优于参与EOP PCC的其他方法; 与IERS A公报相比, 该方法的短期预报效果较好, 当预报跨度增加时预报精度低于IERS A公报. 预报结果表明该方法更适合于极移短期预报.     

A Revisit to the Optical Starlight Polarization Catalogue by Heiles: Distance Update

Starlight polarization serves one of the powerful tools to study magnetic fields in the Galactic interstellar medium. Heiles catalogue contains polarization information for 9286 stars, and is by far the biggest. This catalogue has been extensively used to study the magnetic fields. However, the distance parameters of the stars in this catalogue are from photometric observations, and very uncertain. We cross match Heiles catalogue with Gaia Data Release 2 (DR2), and identify 7613 stars using both angular separation and magnitude as constraints. We then obtain precise distances from Gaia DR2 for these stars. For more than 90% of the stars, the relative errors of the new distances are within 20%. Based on the new catalogue, we demonstrate how starlight polarization can probe Galactic magnetic fields.     

Proper motions in the field of the globular cluster NGC 6934

We measured relative proper motions with a typical accuracy of 1.0 milliarcsec/year (mas/a) for 2000 stars in a 1°4 × 1°4 field around the low-latitude globular cluster NGC 6934. Four plates taken with the Bonn double refractor, spanning an epoch difference of 62 years, were digitized completely. Within the tidal radius of the cluster, we find 106 stars with proper motion errors less than 5 mas/a. Membership probalilities are computed taking into account the individual proper motion errors and the radial distances to the cluster centre. We derive the mean relative proper motion of NGC 6934 using stars with high membership probabilities from radial velocities (Smith and Bell 1986) or from their location in the colour-magnitude diagram (Harris and Racine 1973). The relative proper motions of four Hipparcos stars in the field will be used to obtain the absolute proper motion of NGC 6934 once the extragalactically calibrated Hipparcos Output Catalogue is available.     

1：10000地形图基础测绘产品的质量与检验

结合新疆1：10000基础测绘地形图产品,对质量现状、存在的问题以及如何确保基础测绘地形图产品的质量与确定检验方法,进行了深入探讨。     

Solar diameter measurements at São Paulo Observatory

In this work we describe solar radius measurements made from 1972 with the São Paulo astrolabe. We find values of  959.52 ± 0.03 arcsec  for the visual data and  959.61 ± 0.05 arcsec  for the CCD data using a modified data acquisition system. We compare our results with other astrolabe measurements and with SOHO –MDI. Observations of the solar radius show contradictory results when we try to correlate changes in the diameter with the solar cycle. Our series is not correlated with the solar cycle but it shows a period of  13.4 ± 2.2 yr  . We have also compared our time series with other long-term measurements of solar radius along solar cycle 21 and analysed our measurements as a function of heliographic latitude. We do not find a significant solar oblateness.     

并置VLBI站的相对形变及其与全球解结果的比较

基于ITRF2000地球参考架的三维VLBI站速度矢量和NNR-NUVEL-1A地球板块运动模型，采用观测的VLBI基线长变化率作为约束，估计和讨论了全球6个并置VLBI站的局部或区域性地壳的相对形变，并与国际地球参考架ITRFs解和VLBI全球解glb2003以及VTRF2003的结果进行了比较．结果表明日本Kashima与Kashim34VLBI站之间，美国GREENBANK的NRAO20与NRAO85-3站之间可能存在每年约近4毫米的相对垂直形变；WESTFORD与HAYSTACK二站间每年近2毫米的垂直形变率差基本可得到肯定，KOKEE和KAUAI二站的垂直形变率约有每年1至3毫米的差．利用如下方法能较可靠地检测出并置VLBI站间的局部或区域性的地壳垂直形变，改进ITRF解的可能不足．