基于有限元法的电磁铁磁场的计算机定量分析

随着工程领域中对电磁铁磁场分析的计算精度要求的不断提高,要求有新的数值分析方法以适应这一需求,有限元法即是符合这一需求的分析方法。主要阐述了应用有限元法分析数字阀电磁铁问题的基本思想,并运用该方法对产品前期设计进行了精密的计算和性能预测,节省了大量的设计费用,经济可比性较高。     

一种翼身融合飞行器的失速特性研究

翼身融合（BWB）布局飞行器作为下一代商用飞机的主要构型之一，越来越受到重视。对于翼身融合飞行器的研究主要针对其巡航状态的特性，而对其失速特性的研究较少。对一种翼身融合客机构型进行风洞试验研究，采用测力试验方法对其无增升装置的构型，以及具有翼梢小翼、前缘缝翼和机身上部双吊舱的组合部件构型下的纵向特性进行研究，特别是对其失速特性的分析，并通过二维粒子图像测试技术以及油流试验对其失速过程的流动机理进行研究。结果表明，无增升装置的基本构型下，翼身融合飞行器可以保持低速飞行，而各组合构型都具有提高最大升力系数的作用。对失速过程的分析表明，随着迎角的增大，飞机表面流场分离区域从翼梢开始逐渐向翼根以及机身发展，当外翼段完全处于分离区域时，飞机并不会马上失速，因为中心体同样具有提供升力的作用，且中心体的流动分离较外翼的流动分离更晚，所以当外翼在失速迎角出现升力损失时可以通过中心体的升力进行补偿，维持其低速飞行状态，真正的失速发生在中心体出现流动分离之后。     

Role of scalar fields in cosmological models

Recent astronomical observations of supernovae and cosmic microwave background indicate that the universe is accelerating. Scalar–tensor theories of gravity give rise to suitable cosmological models where a late-time accelerated expansion is naturally realized. In an alternative proposal the cosmic acceleration is generated by means of a scalar field (quintessence), in a way similar to the early-time inflation. In this paper, we consider two classes of cosmological models with scalar fields. The first one corresponds to the Jordan–Brans–Dicke tensor–scalar theory with a cosmological scalar and the second one contains a conformally coupled scalar field with quartic potential. In both type of models the cosmological dynamics is described and the deceleration parameter is evaluated. The values of the parameters are specified for which a late-time accelerated expansion is realized.     

Mid 19th century minimum of galactic cosmic ray flux inferred from Ti in Allegan meteorite

Measurements of ⁴⁴Ti activity in meteorites show that the galactic cosmic ray (GCR) intensity has been declining in the interplanetary space during the past three centuries and has a component of cyclic variation, with periodicity of about 87 years [Taricco, C., Bhandari, N., Cane, D., et al. Galactic cosmic ray flux decline and periodicities in the interplanetary space during the last 3 centuries revealed by ⁴⁴Ti in meteorites. J. Geophys. Res. 111, A08102, 2006.]. In order to verify these results, we have measured ⁴⁴Ti activity in Allegan meteorite which fell in 1899 and in some other meteorites with better precision. The measurements confirm low cosmic ray flux and consequently high solar activity near the middle of 19th century.     

大量程力平衡加速度表的系数标定技术

对比研究了用于加速度表标定的重力场，离心机与电模拟的三种方法，给出了在国内目前没有大ｇ值精密离心机条件下，如何解决大量程加速度表的系数标定问题。     

Recovery of the Earth’s gravity field from formation-flying satellites: Temporal aliasing issues

Temporal and mean gravity field models derived from the twin-satellite, leader–follower mission GRACE have provided a new type of information for Earth sciences. In this contribution, we study the potential of various alternative satellite formations for gravity field determination in the post-GRACE era in a simulation environment. In particular, the effects of spherical harmonic truncation and of temporal aliasing in the processing of gravity products from such future formations are investigated.     

双旋流器单头部模型燃烧室冷态流场试验

利用PIV(Particle image velocimetry)技术对双轴向反旋旋流器、单头部、矩形模型燃烧室内的冷态流场进行了试验研究.分析了燃烧室的纵向截面、横向截面上的流场结构以及旋流器参数对回流区尺寸的影响.研究结果表明:双旋流燃烧室的流场为不规则的结构,中心轴上下两个涡不对称,各主燃孔气流穿透深度也不相同,流场中存在流向涡;减小一级旋流器流通面积、旋流数,或增大二级旋流器的旋流数,可增大回流区的尺寸,而增大二级旋流器流通面积,回流区的尺寸会减小.      

电渣熔铸过程渣池深度对钢锭应力场影响的模拟研究

针对电渣熔铸钢锭各部位温差大,易产生热应力及测量困难,本文采用大型有限元分析软件ANSYS对电渣熔铸过程中不同渣池深度时的钢锭应力场进行了模拟研究,研究结果表明不同渣池深度时的钢锭表面沿轴向自顶而下等效应力和轴向应力分布均基本遵循对数函数关系。模拟结果与实际相吻合,运用此模型可预报钢锭应力场状况,指导实际生产。     

磁扰期间的三维漂移壳分离

基于磁层粒子动力学理论,首先对比了计算漂移壳分离的引导中心法和磁力线追踪法,计算表明两种方法的计算结果一致.然后分别采用T89c和T96磁层磁场模式,用磁力线追踪法数值计算了不同初始位置(≤9Re)、不同初始投掷角、不同Kp指数和不同太阳风压力下,带电粒子的漂移壳分离.计算结果揭示了漂移壳分离随初始位置、投掷角、Kp指数和太阳风压力的变化.其具体特征如下. (1)随着径向距离的增大,漂移壳分离效应愈加显著,由正午出发的粒子将被稳定捕获,而午夜出发的径向距离≥7Re的部分大投掷角粒子将沿磁层顶逃逸. (2)正午出发的粒子,漂移到午夜时其漂移壳随投掷角减小向外排列;午夜出发的粒子,漂移到正午时其漂移壳随投掷角增大排列; 90°投掷角粒子在磁赤道面的漂移壳沿着磁场等值线排列. (3)漂移壳分离随Kp指数和太阳风压力增大变得显著,且随这两种扰动参数的变化特征和趋势是基本相似的.      

Influence of different atmospheric models and seeing effects on the nonlinear calibration

This paper describes a technique intended to improve calibration of vector magnetograms achieved by the spectral line Fei 5324.19 Å which was first described in detail by Hagyard and Kineke [Hagyard, M.J., Kineke, J.I., Improved method for calibrating filter vector magnetographs, Solar Phys., 158, 11–28, 1995.]. The technique attempts to compensate for nonlinear behavior of the measured linear and circular polarizations of the line as functions of inclination angle and field strength. This method depends on different atmospheric models. To the three different atmospheric models, the VAL-C quiet photosphere model, the Ding and Fang penumbra model and Allen umbral model, the circular polarization signal is directly linearly proportional to the longitudinal field strength in the range of 800 G, 1000 G and 1300 G, respectively. For the transverse field, however, this linear relationship holds over much smaller ranges which are 200 G, 300 G and 200 G. The improved method improves the accuracy in calibrating the polarization signals over a wide range of field strengths and inclination angles. With the seeing effects decreasing in the magnetic observation, the longitudinal fields and the transverse ones are underestimated. The differences in the zero-iterative longitudinal and transverse field are relatively minor, but differences in the multi-iterative longitudinal and transverse field can be as high as 260 G and 500 G. The improved calibration method is more sensitive to the seeing effects variation than the former calibration method.