粘性不可压缩流动三维复杂流场分块耦合求解

提出了一个粘性不可压缩流动三维复杂流场的分块耦合求解方法。可解决科学和工程计算中的各种稳态和瞬态粘性不可压缩流动计算问题。     

航空同步发电机的等效磁路模型

分析了航空同步电机的磁路结构特点，建立了电机的等效磁路模型，由等效磁路的拓扑结构导出其磁位非线性方程，再由磁路欧姆定律及铁磁材料的磁化曲线求出其数值解，计算了电机的空载特性和零功率因数负载特性，与实测结果非常接近。     

光时域反射仪检定装置测量不确定度评定

介绍了光时域反射仪检定装置的测量不确定度评定方法,此方法适用于建立计量标准的测量不确定度评定.     

Variations of the magnetic fields in large solar flares

We present preliminary results from high resolution observations obtained with the Michelson Doppler Imager (MDI) instrument on the SOHO of two large solar flares of 14 July 2000 and 24 November 2000. We show that rapid variations of the line-of-sight magnetic field occured on a time scale of a few minutes during the flare explosions. The reversibility/irreversibility of the magnetic field of both active regions is a very good tool for understanding how the magnetic energy is released in these flares. The observed sharp increase of the magnetic energy density at the time of maximum of the solar flare could involve an unknown component which deposited supplementary energy into the system. This revised version was published online in August 2006 with corrections to the Cover Date.     

磁制动对地壳板块运动影响的理论分析与实证研究

太阳和木星的自转是不均匀的，纬度愈高，自转愈慢。据此，作者推测液态外地核的自转，也存在类似的不均匀性，而这种不均匀自转将对地壳板块运动产生影响。利用磁流体力学理论，阐明这类星球自转的不均匀性，是磁制动的不均匀性引起的。研究了磁制动对地壳板块运动影响的途径及表现方式，并举出实例证明这些表现方式的确存在，从而证明磁制动是影响地壳板块运动的一个极为重要的因素。     

Modelling of the electromagnetic field in the interplanetary space and in the Earth's magnetosphere

A magnetohydrodynamic model of the solar wind flow is constructed using a kinematic approach. It is shown that a phenomenological conductivity of the solar wind plasma plays a key role in the forming of the interplanetary magnetic field (IMF) component normal to the ecliptic plane. This component is mostly important for the magnetospheric dynamics which is controlled by the solar wind electric field. A simple analytical solution for the problem of the solar wind flow past the magnetosphere is presented. In this approach the magnetopause and the Earth's bow shock are approximated by the paraboloids of revolution. Superposition of the effects of the bulk solar wind plasma motion and the magnetic field diffusion results in an incomplete screening of the IMF by the magnetopause. It is shown that the normal to the magnetopause component of the solar wind magnetic field and the tangential component of the electric field penetrated into the magnetosphere are determined by the quarter square of the magnetic Reynolds number. In final, a dynamic model of the magnetospheric magnetic field is constructed. This model can describe the magnetosphere in the course of the severe magnetic storm. The conditions under which the magnetospheric magnetic flux structure is unstable and can drive the magnetospheric substorm are discussed. The model calculations are compared with the observational data for September 24–26, 1998 magnetic storm (Dst _min=−205 nT) and substorm occurred at 02:30 UT on January 10, 1997. This revised version was published online in August 2006 with corrections to the Cover Date.     

Relationship Between Substorm Auroras and Processes in the Near-Earth Magnetotail

Although the auroral substorm has been long regarded as a manifestation of the magnetospheric substorm, a direct relation of active auroras to certain magnetospheric processes is still debatable. To investigate the relationship, we combine the data of the UV imager onboard the Polar satellite with plasma and magnetic field measurements by the Geotail spacecraft. The poleward edge of the auroral bulge, as determined from the images obtained at the LHBL passband, is found to be conjugated with the region where the oppositely directed fast plasma flows observed in the near-Earth plasma sheet during substorms are generated. We conclude that the auroras forming the bulge are due to the near-Earth reconnection process. This implies that the magnetic flux through the auroral bulge is equal to the flux dissipated in the magnetotail during the substorm. Comparison of the magnetic flux through the auroral bulge with the magnetic flux accumulated in the tail lobe during the growth phase shows that these parameters have the comparable values. This is a clear evidence of the loading–unloading scheme of substorm development. It is shown that the area of the auroral bulge developing during substorm is proportional to the total (magnetic plus plasma) pressure decrease in the magnetotail. These findings stress the importance of auroral bulge observations for monitoring of substorm intensity in terms of the magnetic flux and energy dissipation.     

应用于磁悬挂系统的200V─6OA晶体管斩波器

在大功率磁悬挂系统中，电磁铁电流必须采用开关频率较高的大功率斩波器来调节。本文介绍一个用于磁悬挂系统的大功率晶体管斩波器，它的工作电源电压为２００Ｖ，输出电流为６０Ａ，斩波频率为２ｋＨｚ，试验负载从阻性到感性，电感量达２．５Ｈ。该斩波器在一个单自由度大功率磁悬浮试验装置中完成了磁悬挂控制试验。该斩波器由不对称半桥、开关辅助网络、最优基极驱动电路ＵＡＡ４００２、一次脉冲源ＭＣ３４０６０及电流反馈环等部分构成，具有多种保护功能和良好的传输特性线性度。     

有效载荷／运载火箭耦合分析的频域方法

盘算尖响函数综合技术导出了用耦合频响函数和无有效载荷的运载火箭界面加速度响应表示的有效载荷／运载火箭耦合动力分析的频域方法，给出了以自由界面的运载火箭模态分数放自由界面或固定界面有效载荷模态参数构成的耦合频响函数表达式。     

五自由度磁悬磨头电控系统研究

研究的高速磨床电磁悬浮磨头电控系统尽量采用最新技术，在保证系统 性能的前提下降低了系统造价。在该系统中采用TMS320F240 DSP芯片作为控制核心，同时控制磁悬浮轴承的悬浮和变频电机调速，采用运行效率很高的汇编语言编写控制软件，其中磁悬浮轴承是PID控制算法，电机调速为SPWM方式。磁悬浮轴承PWM功率放大器中采用能简化驱动的新型半桥电路，电机调速主电路中采用智能功率模块（IPM）。动态刚度测试和高速运转实验表明，该电控系统满足高速磨床电磁悬浮磨头的控制要求。