基于dSPACE的永磁同步电机低振动噪声控制策略

为降低变频器供电引起的永磁同步电机(PMSM)电磁振动噪声,首先理论分析了变频器引入的PMSM振动噪声源,然后利用MATLAB/Simulink建立仿真模型,通过dSPACE进行编译并控制一台PMSM,比较了随机开关频率调制技术和死区补偿技术降低振动噪声的优缺点,提出一种混合随机开关频率死区补偿技术。试验结果表明,此方法综合随机开关频率调制技术和死区补偿技术的优点,能降低逆变器引入电流谐波引起的中低频振动噪声和逆变器开关频率与电流谐波相互作用引起的高频振动噪声。     

Modeling the (upper) solar atmosphere including the magnetic field

The atmosphere of the Sun is highly structured and dynamic in nature. From the photosphere and chromosphere into the transition region and the corona plasma-β changes from above to below one, i.e., while in the lower atmosphere the energy density of the plasma dominates, in the upper atmosphere the magnetic field plays the governing role – one might speak of a “magnetic transition”. Therefore the dynamics of the overshooting convection in the photosphere, the granulation, is shuffling the magnetic field around in the photosphere. This leads not only to a (re-)structuring of the magnetic field in the upper atmosphere, but induces also the dynamic reaction of the coronal plasma, e.g., due to reconnection events. Therefore the (complex) structure and the interaction of various magnetic patches is crucial to understand the structure, dynamics and heating of coronal plasma as well as its acceleration into the solar wind.

The present article will emphasize the need for three-dimensional modeling accounting for the complexity of the solar atmosphere to understand these processes. Some advances on 3D modeling of the upper solar atmosphere in magnetically closed as well as open regions will be presented together with diagnostic tools to compare these models to observations. This highlights the recent success of these models which in many respects closely match the observations.     

Using LASCO-C1 spectroscopy for coronal diagnostics

The LASCO-C1 telescope was designed to perform spectral analysis of coronal structures by means of a tunable Fabry–Pérot interferometer acquiring images at different wavelengths. Results from spectral scans of the Fe xiv 5303 Å green coronal emission line are presented. Physical quantities like the ion temperature (line widths), and the flow velocity along the line of sight (Doppler shifts) are obtained over the entire corona.     

基于变增益扩张状态观测器的永磁同步电机转速环自抗扰控制器设计

线性扩张状态观测器(LESO)在观测初始阶段,系统状态量实际值与估计值误差较大。由于LESO高增益的影响,导致LESO在初始时刻的扰动估计输出出现很大的峰值,而且观测器增益越大,峰值现象越严重。针对上述问题,设计了一种变增益扩张状态观测器(TESO),其增益是一个时变函数,在初始时刻为较小的函数值,随着时间逐渐增大,直至趋于一个较大常数。利用李雅普诺夫变换和微分代数谱理论给出了参数整定公式。将线性自抗扰控制器(LADRC)中的扩张状态观测器替换为TESO,并将其应用于永磁同步电机转速控制中,计算机仿真和系统试验验证了该控制器设计的有效性。     

永磁辅助式同步磁阻电机转矩预测控制方法

为了验证永磁磁阻电机具备宽调速域的优势,同时充分发挥永磁磁阻电机在弱磁运行时的输出转矩,提出了一种基于转矩预测控制的全速域控制方法。采用Ansys设计了一台永磁磁阻电机,并与Simulink联合仿真验证了方法的可行性。验证结果表明:转矩预测控制方法可以使电机在全速域获得良好的动态性能,同时永磁磁阻电机弱磁运行时依然具有优秀的转矩输出能力。     

“风云”系列气象卫星的发展现状及其展望

介绍了我国第一代极地气象卫星“风云一号”（FY－1）系列和静止气象卫星“风云二号”（FY－2）系列的发展历程、主要性能。FY－1系列包括4颗卫星及其相应的地面数据接收、处理和应用系统。介绍了FY－2后续卫星及FY-3的发展计划。最后还介绍了遥感卫星遥感器辐射校正场计划。     

充磁导致的超高速永磁同步电机不平衡磁拉力

转子永磁体充磁角度偏差导致的不平衡磁拉力对微型燃气轮机发电系统用超高速永磁同步电机的安全稳定运行有很大的影响.采用有限元数值分析方法,分别在不考虑转子偏心和考虑转子偏心的情况下,对由充磁角度偏差导致的超高速永磁同步电机不平衡磁拉力进行了计算和分析;将不平衡磁拉力的计算结果作为载荷,获得了超高速永磁同步电机空气轴承-转子系统的固有频率及振动特性.研究结果表明:转子系统在740 Hz附近发生共振,共振幅值随着转子磁芯充磁偏差角度的增大而增大;要保证转子系统安全可靠的工作,需要将磁芯的充磁角度偏差限制在5°以内.     

计及开关频率优化的永磁同步电机模型预测转矩控制

为减小逆变器开关频率对永磁同步电机(PMSM)性能的影响,提出了一种计及开关频率优化的PMSM模型预测转矩控制(MPTC)方法。建立了电磁转矩及定子磁链数学模型,并在此基础上设计了MPTC全速域价值函数。在全速域价值函数中加入了逆变器开关频率的限制条件,以实现恒转矩区内最大转矩电流比、恒功率区内弱磁调速并计及开关频率最优化的控制效果。仿真结果证明了所提方案不仅具有较高的动态响应性能,而且有效降低了逆变器的开关频率。     

基于同伦函数的直驱永磁同步风电机组次同步振荡特征值分析

为了研究直驱永磁同步风电机组的次同步振荡问题,建立了典型的风电系统数学模型。在使用传统特征值分析法的基础上,利用同伦函数代替参与因子法,准确且直观地辨识出系统振荡模态特征值对应的状态变量。在此基础上进一步分析状态变量对应的参数对系统振荡模态特征值的影响。最后,通过PSCAD/EMTDC平台进行时域仿真。结果表明:直流电压控制外环积分系数和电流控制内环比例系数对系统的次同步振荡有很大影响。     

Probing the method of correcting Faraday rotation in vector magnetograms

By analyzing the vector magnetograms of Huairou Solar Observing Station (HSOS) taken at the line center (0.0 Å) and the line wing (−0.12 Å) of FeI λ5324.19 Å, we make an estimate of the measured errors in transversal azimuths (δ?) caused by Faraday rotation. Since many factors, such as the magnetic saturation and scattered light, can affect the measurement accuracy of the longitudinal magnetic field in the umbrae of sunspots, we limit our study in the region ∣B_z∣ < 800 G. The main mean azimuth rotations are about 4°, 6°, 7° and 9°, while ∣B_z∣ are in the ranges of 400–500 G, 500–600 G, 600–700 G and 700–800 G, respectively. Moreover, we find there is also an azimuth rotation of about 8° at the wavelength offset −0.12 Å of the line compared against a previous numerical simulation.