盘式永磁同步电机永磁体涡流损耗研究

由于永磁体中存在涡流损耗,这些损耗会以热量的形式散发出来,使盘式永磁同步电机(DPMSM)内部温度升高。当温度过高时,会引起电机运行性能降低。故针对永磁体涡流损耗进行深入研究,对DPMSM的性能提高及优化设计具有重要意义。利用Maxwell三维电磁场有限元分析软件建立电机有限元模型,在三相正弦电流源驱动下求解电机永磁体电磁场分布;为减小永磁体涡流损耗,对永磁体进行不同方向分割,并对不同方向分割进行仿真对比,得出横向分割为3块效果最佳;在利用电磁屏蔽原理减小涡流损耗时,先对其可靠性进行验证,后利用MATLAB曲线拟合得出屏蔽层厚度的最优值。     

一种卡尔曼滤波器的永磁同步电机无速度传感器

针对滑模观测器的永磁同步电机参数误差容易造成估算误差和反电动势中存在高频纹波分量的缺点,使用低通滤波器不能有效消除高频纹波,提出在滑模观测器前端引入卡尔曼滤波器来消除高频纹波,使得永磁同步电机的控制系统具有更好的稳态效果和动态响应。依据设计仿真搭建MATLAB平台,对提出新方法进行验证。试验结果表明增加卡尔曼滤波环节后的滑模观测器不仅鲁棒性强,而且在一定程度上有效抑制了抖振,在系统快速性及稳态性能上都有较好的效果。     

基于最小二乘法和硬件在环平台的永磁同步电机参数辨识

针对永磁同步电机多个参数同时辨识时会出现欠秩的情况,介绍了在dq坐标系下采用最小二乘法将多个参数分开辨识的方法。在硬件在环平台上采用该方法对电阻、电感和磁链进行了辨识。最后进一步考虑到电阻和磁链受温度的影响较大,进行了考虑温升的电阻和磁链的辨识。经验证,该方法可以比较准确地辨识出电机参数。     

Luenberger观测器在永磁同步电机无传感器控制中的应用研究

在永磁同步电机(PMSM)矢量控制中,根据Luenberger观测器原理,提出了一种基于Luenberger观测器的PMSM转子速度和位置的估算方法,有效解决了PMSM由于机械传感器安装带来的一些弊端。利用MATLAB/Simulink工具搭建控制系统仿真模型并进行仿真验证,仿真结果表明控制系统具有良好的控制性能。最后,在以STM32F103ZET6为控制核心的硬件系统上进行算法的实现,试验结果表明基于Luenberger观测器的PMSM控制系统具有较高的控制精度且稳定性较好。     

The gas pixel detector as a solar X-ray polarimeter and imager

The Sun is the nearest astrophysical source with a very intense emission in the X-ray band. The study of energetic events, such as solar flares, can help us to understand the behaviour of the magnetic field of our star. There are in the literature numerous studies published about polarization predictions, for a wide range of solar flares models involving the emission from thermal and/or non-thermal processes, but observations in the X-ray band have never been exhaustive.The gas pixel detector (GPD) was designed to achieve X-ray polarimetric measurements as well as X-ray images for far astrophysical sources. Here we present the possibility to employ this instrument for the observation of our Sun in the X-ray band.     

Variations of the solar acoustic high-degree mode frequencies over solar cycle 23

Using full-disk observations obtained with the Michelson Doppler Imager (MDI) on board the Solar and Heliospheric Observatory (SOHO) spacecraft, we present variations of the solar acoustic mode frequencies caused by the solar activity cycle. High-degree (100 < ? < 900) solar acoustic modes were analyzed using global helioseismology analysis techniques over most of solar cycle 23. We followed the methodology described in details in [Korzennik, S.G., Rabello-Soares, M.C., Schou, J. On the determination of Michelson Doppler Imager high-degree mode frequencies. ApJ 602, 481–515, 2004] to infer unbiased estimates of high-degree mode parameters ([see also Rabello-Soares, M.C., Korzennik, S.G., Schou, J. High-degree mode frequencies: changes with solar cycle. ESA SP-624, 2006]). We have removed most of the known instrumental and observational effects that affect specifically high-degree modes. We show that the high-degree changes are in good agreement with the medium-degree results, except for years when the instrument was highly defocused. We analyzed and discuss the effect of defocusing on high-degree estimation. Our results for high-degree modes confirm that the frequency shift scaled by the relative mode inertia is a function of frequency and it is independent of degree.     

Element Separation in the Chromosphere Ionization-Diffusion Models for the FIP-Effect

Ionization-diffusion mechanisms to understand the first ionization potential (FIP) fractionation as observed in the solar corona and the solar wind are reviewed. The enrichment of the low-FIP elements (<10 eV) compared to the high-FIP elements, seen in e.g. slow and fast wind or polar plumes, is explained. The behaviour of the heavy noble gases becomes understandable. The absolute fractionation, i.e. in relation to hydrogen, can be calculated and fits well to the measurements. The theoretical velocity-dependence of the fractionation will with used to determine the velocities of the solar wind in the chromosphere. This revised version was published online in June 2006 with corrections to the Cover Date.     

Radial profile measurements of the solar wind speed using radio sounding techniques

Velocity measurements of the solar wind in the region of its acceleration were carried out in 1984 with Venera Orbiters using the following specific radio sounding techniques: (i) phase and frequency correlations from two or three widely-spaced ground stations; (ii) phase and frequency correlations from two spacecraft and two widely-spaced ground stations; (iii) two station two-way coherent Doppler measurements; (iv) determination of the break frequency in power spectra of intensity fluctuations. Our results are substantially lower than those derived from direct Doppler shift measurements of transition region and lower coronal resonance lines and those from measurements applying the Doppler dimming technique.     

Probing solar and stellar interior dynamics and dynamo

Solar and stellar activity is a result of complex interaction between magnetic field, turbulent convection and differential rotation in a star’s interior. Magnetic field is believed to be generated by a dynamo process in the convection zone. It emerges on the surface forming sunspots and starspots. Localization of the magnetic spots and their evolution with the activity cycle is determined by large-scale interior flows. Thus, the internal dynamics of the Sun and other stars hold the key to understanding the dynamo mechanism and activity cycles. Recently, significant progress has been made for modeling magnetohydrodynamics of the stellar interiors and probing the internal rotation and large-scale dynamics of the Sun by helioseismology. Also, asteroseismology is beginning to probe interiors of distant stars. I review key achievements and challenges in our quest to understand the basic mechanisms of solar and stellar activity.     

The Seed Population for Energetic Particles Accelerated by CME-Driven Shocks

Understanding properties of solar energetic particle (SEP) events associated with coronal mass ejections has been identified as a key problem in solar-terrestrial physics. Although recent CME shock acceleration models are highly promising, detailed agreement between theoretical predictions and observations has remained elusive. Recent observations from ACE have shown substantial enrichments in the abundances of ³He and He⁺ ions which are extremely rare in the thermal solar wind plasma. Consequently, these ions act as tracers of their source material, i.e., ³He ions are flare suprathermals and He⁺ ions are interstellar pickup ions. The average heavy ion composition also exhibits unsystematic differences when compared with the solar wind values, but correlates significantly with the ambient suprathermal material abundances. Taken together these results provide compelling evidence that CME-driven shocks draw their source material from the ubiquitous but largely unexplored suprathermal tail rather than from the more abundant solar wind peak. However, the suprathermal energy regime has many more contributors and exhibits much larger variability than the solar wind, and as such needs to be investigated more thoroughly. Answers to fundamental new questions regarding the preferred injection of the suprathermal ions, the spatial and temporal dependence of the various sources, and the causes of their variability and their effects on the SEP properties are needed to improve agreement between the simulations and observations.