裁剪曲面的参数线加工算法研究

结合开发国产化软件的实践，详细论述了ＣＡＤ／ＣＡＭ技术中有关裁剪曲面的描述及加工自动编程算法的研究。从曲面造型及加工编程的通用性角度出发，将曲面的三维几何信息映射到二维参数域上，用二维拓扑信息环来描述裁剪曲面，把各种裁剪曲面的加工编程统一为一种具有拓扑信息环的广义曲面加工编程。同时，采用环形刀计算刀位信息，可方便地推广至球头刀或平底刀的加工编程。根据预先设定的残留高度及插补误差，在编程中对刀切点和刀位点的计算进行有效控制，保证了加工编程的精度要求。从而用较简单的方法实现了对任意裁剪曲面的加工自动编程     

交—交型矩阵变换器的双电压控制原理及波形合成

介绍了一般意义上的ｎ×ｍ型矩阵变换器的拓扑形式及双向功率开关的构成；分析了基于瞬时电压调制技术的三相ＡＣ－ＡＣ矩阵变换器的开关状态和控制规律；给出了在一个周期里，划分输入相区，输出相区的原则，从理论上推出了改进的双线电压控制的矩阵变换器的控制函数表达式。     

一种基于实体模型的三轴数控加工刀轨生成算法

实体模型是几何造型的高级模型，它具有完整的曲面拓扑关系，国内基本实体模型的数摈加工算法的需求日渐迫切，本文提出了一种适合实体模型的三轴数控加工刀位轨迹生成算法；首先根据加工行距作一组平行于刀轴的平面，与模型的待加工表面求交，得到一系列交线，再根据加工步长规划另一组与上述平面垂直且平行于刀轴的平面，与上述交线求交，得到一交点网格，判断刀具与数据点的位置关系从而得到刀位轨迹。     

Data Association and Track Management for the Gaussian Mixture Probability Hypothesis Density Filter

The Gaussian mixture probability hypothesis density (GM-PHD) recursion is a closed-form solution to the probability hypothesis density (PHD) recursion, which was proposed for jointly estimating the time-varying number of targets and their states from a sequence of noisy measurement sets in the presence of data association uncertainty, clutter, and miss-detection. However the GM-PHD filter does not provide identities of individual target state estimates, that are needed to construct tracks of individual targets. In this paper, we propose a new multi-target tracker based on the GM-PHD filter, which gives the association amongst state estimates of targets over time and provides track labels. Various issues regarding initiating, propagating and terminating tracks are discussed. Furthermore, we also propose a technique for resolving identities of targets in close proximity, which the PHD filter is unable to do on its own.     

DS CATIA V6让扁平的世界立起来——访达索系统大中华区总经理赵恒先生

[编者按]当弗里德曼关于"世界是平的"的断言还余音犹存时,现实已经开始完全向相反的方向变化:近日,全球PLM领域的领导厂商达索系统公司推出了新一代的PLM2.0战略和CATIA V6平台.     

Characteristics of Icy Surfaces

The surfaces of the Solar System’s icy satellites show an extraordinary variety of morphological features, which bear witness to exchange processes between the surface and subsurface. In this paper we review the characteristics of surface features on the moons of Jupiter, Saturn, Uranus and Neptune. Using data from spacecraft missions, we discuss the detailed morphology, size, and topography of cryovolcanic, tectonic, aeolian, fluvial, and impact features of both large moons and smaller satellites.     

Implications of X-ray Observations for Electron Acceleration and Propagation in Solar Flares

High-energy X-rays and ??-rays from solar flares were discovered just over fifty years ago. Since that time, the standard for the interpretation of spatially integrated flare X-ray spectra at energies above several tens of keV has been the collisional thick-target model. After the launch of the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) in early 2002, X-ray spectra and images have been of sufficient quality to allow a greater focus on the energetic electrons responsible for the X-ray emission, including their origin and their interactions with the flare plasma and magnetic field. The result has been new insights into the flaring process, as well as more quantitative models for both electron acceleration and propagation, and for the flare environment with which the electrons interact. In this article we review our current understanding of electron acceleration, energy loss, and propagation in flares. Implications of these new results for the collisional thick-target model, for general flare models, and for future flare studies are discussed.     

带探针装置的倾斜卧式椭直圆筒罐罐容表函数的计算

针对带探针装置的倾斜卧式椭直圆筒罐罐容表函数(即罐内储油量与探针油位高度对应的函数关系)的理论计算问题,首先采用"冰冻"思维和相对运动等效地把倾斜卧式的情形转化为水平卧式的情形,然后根据液面与关键液面的不同位置关系采取了不同的计算方法,最后分段地得到了罐容表函数的一般表达式。     

Longitudinal variation of the equatorial ionosphere: Modeling and experimental results

We describe a new version of the Parameterized Regional Ionospheric Model (PARIM) which has been modified to include the longitudinal dependences. This model has been reconstructed using multidimensional Fourier series. To validate PARIM results, the South America maps of critical frequencies for the E (foE) and F (foF2) regions were compared with the values calculated by Sheffield Plasmasphere-Ionosphere Model (SUPIM) and IRI representations. PARIM presents very good results, the general characteristics of both regions, mainly the presence of the equatorial ionization anomaly, were well reproduced for equinoctial conditions of solar minimum and maximum. The values of foF2 and hmF2 recorded over Jicamarca (12°S; 77°W; dip lat. 1°N; mag. declination 0.3°) and sites of the conjugate point equatorial experiment (COPEX) campaign Boa Vista (2.8°N; 60.7°W; dip lat. 11.4°; mag. declination −13.1°), Cachimbo (9.5°S; 54.8°W; dip lat. −1.8°; mag. declination −15.5°), and Campo Grande (20.4°S; 54.6°W; dip lat. −11.1°; mag. declination −14.0°) have been used in this work. foF2 calculated by PARIM show good agreement with the observations, except during morning over Boa Vista and midnight-morning over Campo Grande. Some discrepancies were also found for the F-region peak height (hmF2) near the geomagnetic equator during times of F₃ layer occurrences. IRI has underestimated both foF2 and hmF2 over equatorial and low latitude sectors during evening-nighttimes, except for Jicamarca where foF2 values were overestimated.     

A statistical study of C IV regions in 20 Oe-stars

In this paper, using the Gauss-Rotation model (GR model), we analyse the UV C IV resonance lines in the spectra of 20 Oe-stars of different spectral subtypes, in order to detect the structure of C IV region. We study the presence and behavior of absorption clouds and analyse their characteristics. From this analysis we can calculate the values of a group of physical parameters, such as the apparent rotational and radial velocities, the random velocities of the thermal motions of the ions, the Full Width at Half Maximum (FWHM), the optical depth, as well as the absorbed energy and the column density of the independent regions of matter, which produce the main and the satellite clouds of the studied spectral lines. Finally, we present the relations between these physical parameters and the spectral subtypes of the studied stars and we give our results about the structure of the C IV region in their atmosphere.