实心圆柱式永磁同步电机转子偏心气隙磁场的空间和频率特性

针对两极平行充磁实心圆柱式永磁同步电机(SCPMSM),分析转子偏心对气隙磁场空间和频率特性的影响。通过引入转子静态偏心和动态偏心磁导修正系数,建立了转子偏心气隙磁场的数学模型,分析了空载和负载情形下转子静态偏心以及动态偏心气隙磁场的空间和频率特性。以1台2极12槽SCPMSM为例,对转子偏心气隙磁场特性进行了有限元分析,验证了理论分析的正确性。     

限制转子电流的双馈风电机组虚拟同步控制策略

随着新能源的大规模开发利用,其在能源结构中的占比不断提高。为了维持大电网的平稳运行,要求双馈风机等新能源机组参与电网调频。双馈风机的转子侧变流器存在容量限制,而调频过程中转子电流变化可能会超出此限。为应对这一问题,首先分析了双馈风力发电机的数学模型,并得出了额定转速下dq系的转子电流控制模型;然后使用误差转化函数与李雅普诺夫方法,设计了限制转子电流的控制器,并与常规的虚拟同步控制相结合,提出了一种改进的虚拟同步控制策略,可以兼顾风机调频的需求与调频动态过程中转子电流的限制。通过仿真验证了所提出控制器参与电网调频的能力以及对于转子电流的良好控制。     

采用定子电流与扰动观测的永磁同步电机改进预测电流控制

提出了一种采用定子电流和扰动观测补偿的改进预测电流控制(PCC)算法。理论上永磁同步电机PCC具有优异的控制性能,但现实系统中离散采样延时与电磁参数时变等问题使得原理上基于模型的预测电流控制器的控制品质严重恶化。设计了龙伯格(Luenberger)状态观测器实现对定子电流与参数扰动的观测,并应用于补偿和改进经典的无差拍预测电流控制器。将观测到的当前时刻的定子电流替代当前时刻的采样电流用于反馈控制,以补偿采样延时;运行过程中电磁参数的变化使得模型参数失配,其影响以电压扰动的形式被观测出来,并补偿到预测控制输出的电压指令中。仿真和试验结果验证了所提方法的有效性。     

永磁同步电机全域温度场分析与水道优化设计

以额定功率为60 kW永磁同步电机(PMSM)为研究对象,采用气隙等效导热系数处理定转子间的热交换问题。给出散下线定子绕组的等效热模型。在进行绕组铜耗计算时考虑温升对定子绕组阻值的影响,试验测定壳体与定子铁心间因装配间隙而产生的热阻值。在此基础上建立PMSM三维全域瞬态温度场有限元模型,计算电机在峰值转速运行时的温度场变化,并进行试验验证。对水道宽度比、水道数和翅片进行优化计算,找出最优解。结果表明,水道优化后电机最高温度下降9.8 ℃,对电机水道结构设计具有一定的指导意义。     

逆变器并联驱动永磁同步电机容错控制研究

为了提高逆变器并联驱动永磁同步电机(PMSM)系统的运行可靠性,基于对比研究方式设计了两种逆变器并联驱动PMSM的容错控制方案,分别为正常通路电流补偿方案和等效电流补偿方案。两种容错控制方案均不同于传统方案,后者将故障逆变器整体隔离,前者则充分利用了所有逆变器非故障桥臂,以降低故障条件下的铜耗,并输出平稳转矩。此外,两种新型容错控制方案均结合了比例谐振电流控制器以实现对不对称参考电流的跟踪,避免了并联逆变器之间可能出现的环流。最后,通过PMSM并联驱动系统的容错控制试验,验证了新型容错控制策略的效果。     

Very low thrust station-keeping for low Earth orbiting satellites

Traditional station-keeping for Earth observation satellites with chemical thrusters generally involves maneuvers every couple months that are able to change significantly the semi-major axis and the inclination. These strategies do not scale down to very low thrust level (a few hundreds of μN) electrical thrusters. This paper presents both in-plane and out-of-plane strategies that spread corrections over very long arcs and discretize them to tiny maneuvers every couple orbits, taking into account mission-constraints on maneuvers locations. These strategies scale up to medium thrust strategies, filling the gap between propulsion technologies. The out-of-plane strategy although features a new no-deadband property and controls the full orbital momentum. All strategies allow control very close to the reference (a few hundreds meters in osculating parameters) and very low cost.     

Dynamic neighborhood genetic learning particle swarm optimization for high-power-density electric propulsion motor

To maximize the power density of the electric propulsion motor in aerospace application, this paper proposes a novel Dynamic Neighborhood Genetic Learning Particle Swarm Optimization (DNGL-PSO) for the motor design, which can deal with the insufficient population diversity and non-global optimal solution issues. The DNGL-PSO framework is composed of the dynamic neighborhood module and the particle update module. To improve the population diversity, the dynamic neighborhood strategy is first proposed, which combines the local neighborhood exemplar generation mechanism and the shuffling mechanism. The local neighborhood exemplar generation mechanism enlarges the search range of the algorithm in the solution space, thus obtaining high-quality exemplars. Meanwhile, when the global optimal solution cannot update its fitness value, the shuffling mechanism module is triggered to dynamically change the local neighborhood members. The roulette wheel selection operator is introduced into the shuffling mechanism to ensure that particles with larger fitness value are selected with a higher probability and remain in the local neighborhood. Then, the global learning based particle update approach is proposed, which can achieve a good balance between the expansion of the search range in the early stage and the acceleration of local convergence in the later stage. Finally, the optimization design of the electric propulsion motor is conducted to verify the effectiveness of the proposed DNGL-PSO. The simulation results show that the proposed DNGL-PSO has excellent adaptability, optimization efficiency and global optimization capability, while the optimized electric propulsion motor has a high power density of 5.207 kW/kg with the efficiency of 96.12%.     

Where is the base of the Transition Region? Evidence from TRACE,SDO, IRIS and ALMA observations

Classic solar atmospheric models put the Chromosphere-Corona Transition Region (CCTR) at $～2$ Mm above the ${\tau }_{5000}=1$ level, whereas radiative MHD (rMHD) models place the CCTR in a wider range of heights. However, observational verification is scarce. In this work we review and discuss recent results from various instruments and spectral domains. In SDO and TRACE images spicules appear in emission in the 1600, 1700 and 304 Å bands and in absorption in the EUV bands; the latter is due to photo-ionization of H i and He i, which increases with wavelength. At the shortest available AIA wavelength and taking into account that the photospheric limb is $～0.34$ Mm above the ${\tau }_{5000}=1$ level, we found that CCTR emission starts at $～3.7$ Mm; extrapolating to $\lambda =0$, where there is no chromospheric absorption, we deduced a height of $3.0\pm 0.5$ Mm, which is above the value of 2.14 Mm of the Avrett and Loeser model. Another indicator of the extent of the chromosphere is the height of the network structures. Height differences produce a limbward shift of features with respect to the position of their counterparts in magnetograms. Using this approach, we measured heights of $0.14\pm 0.04$ Mm (at 1700 Å), $0.31\pm 0.09$ Mm (at 1600 Å) and $3.31\pm 0.18$ Mm (at 304 Å) for the center of the solar disk. A previously reported possible solar cycle variation is not confirmed. A third indicator is the position of the limb in the UV, where IRIS observations of the Mg ii triplet lines show that they extend up to $～2.1$ Mm above the 2832 Å limb, while AIA/SDO images give a limb height of $1.4\pm 0.2$ Mm (1600 Å) and $5.7\pm 0.2$ Mm (304 Å). Finally, ALMA mm-$\lambda$ full-disk images provide useful diagnostics, though not very accurate, due to their relatively low resolution; values of $2.4\pm 0.7$ Mm at 1.26 mm and $4.2\pm 2.5$ Mm at 3 mm were obtained. Putting everything together, we conclude that the average chromosphere extends higher than homogeneous models predict, but within the range of rMHD models..     

Evolutionary features of polar and non-polar coronal holes during solar cycle 24 and the rising phase of cycle 25

This paper presents the results of the analysis of the evolution of coronal holes (CHs) on the Sun during the period May 13, 2010 – March 20, 2022, covering Solar Cycle 24. Our study uses images in the extreme-ultraviolet iron line (Fe XII 193 Å) obtained with the Atmospheric Imager Assembly of the Solar Dynamics Observatory (AIA/SDO). To localize CHs and determine their areas, we used the Heliophysics Event Knowledgebase (HEK). We separate the CHs into polar and non-polar and study the evolutionary features of each group. During this period, an asymmetry between the Northern (N) and Southern (S) Hemispheres (N-S or hemispheric asymmetry) is detected both in the solar activity (SA) indices and in the localization of the maximum areas of the polar and non-polar CHs. It is shown that the hemispheric asymmetry of the areas of polar and non-polar CHs varies significantly over time and that the nature of these changes is clearly related to the SA cycle. We find that for most of the period, the polar CHs were predominated generated in the S- hemisphere while the non-polar CHs were dominant in the N- hemisphere. It is found that the maximum and minimum of the hemispheric imbalance in the areas of non-polar CHs are close in time to the maximum and minimum of the asymmetry of the SA indices (the number and areas of sunspots). The maximum hemispheric imbalance of the polar CH areas is observed at the maximum of Cycle 24, and the minimum imbalance is found at the cycle minimum. These results confirm our assumption that these two types of CHs are of a different nature and that the non-polar CHs, like sunspots, are elements of the general magnetic activity.     

Decline of geomagnetic and ionospheric activity at earthquake during spotless Sun

We investigate the geomagnetic and ionospheric effects of seismic activity during 1954 Sun spotless days (SSL) from 1995 to 2020. Two subsets of earthquakes (EQ) are evaluated for 676 events observed with the depth D1 ≤ 30 km and 1278 events with D2 > 30 km and the total set SSL. Newly developed 1 h geomagnetic index Hpo and the ionospheric W_EQ index are used for the comparisons with the daily peak earthquake. The ionosphere W_EQ index is derived at the EQ epicenter from JPL GIM-TEC map within the cell of 2.5°×5°, in latitude φ and longitude λ surrounding the epicenter at radius of about 200 km. We use the method of superposed epoch with the zero epoch time t₀ taken at EQ to extract peak values of Hpo and W_EQ during t₀-24 h ≤ t < t₀ (preEQ) and t₀ < t ≤ t₀ + 24 h (postEQ). It is found that the magnitude of Hpo(t₀) is less that the both peaks of Hpo(preEQ) and Hpo(postEQ) in 91 % of events independent of EQ’s depth. Similar effect is observed with the peak of the positive/negative ionosphere indices and the absolute values of |W(preEQ)| and |W(postEQ)| the both exceeding |W_EQ| in 77 % of events. The seismic activity tends to increase towards the solar minimum when SSLs occur. Our results provide evidence that EQ-related geomagnetic and ionospheric activities experience decline of intensity at the time of EQ under SSL.