计及多因素影响的永磁电机空载气隙磁密解析计算法

为准确而快速地计算与评估电机的性能,以I型转子结构永磁电机为例,提出了一种计及多因素影响的空载气隙磁密的解析计算法,并用有限元进行了仿真验证。分析了永磁体尺寸、隔磁桥高度和极弧系数等参数对气隙磁密的影响规律,为优化电机方案提供了思路。     

基于等效时间的混合储能系统高功率密度优化配置

越来越多的电力电子装置应用到多电飞机（MEA）电力系统中,导致MEA用电负荷功率呈现脉动特性,采用混合储能系统（HESS）平抑负荷功率脉动。为减少HESS重量,提出了一种高功率密度的优化配置方法。为建立负荷功率与储能介质之间的关系,提出了等效时间（ET）的概念,比较两者的ET常数作为储能系统类型选取的依据。进一步提出空间矢量法,采用能量型储能介质矢量和功率型储能介质矢量合成负荷功率,确定最优单体和截止频率,实现了HESS高功率密度配置。同时,从能量约束和功率约束两个方面进行HESS的容量的计算。最后,通过算例配置和仿真分析验证了本文所提方法的可行性和正确性。     

利用经验正交函数分解的大气密度模式校准方法

热层大气密度产生的阻力是作用在低轨航天器上最大的非引力摄动,现有大气密度模式存在15%~20%的偏差,难以满足空间任务应用需要。采用NRLMSISE-00模式作为密度参考标准,通过修正Jacchia-Roberts经验大气模式温度参数校准密度,建立温度修正量与密度的参数方程。针对部分区域修正量迭代计算发散问题,采用改进高斯牛顿迭代法求解方程。选择经验正交函数（EOF）分解方法分析修正量的时空特征,并与传统球谐（SH）分析的结果进行比较。结果表明,前4阶EOF基函数与前9项球谐基函数分别可提取温度修正量超过85%与80%的变化特征,EOF分解方法对温度修正量的表示效率高于球谐分析方法。第1阶EOF基函数反映了温度参数的整体偏差,第2~4阶EOF基函数对应的时间系数表明温度修正量的变化具有天周期性,且球谐分析得到的时间系数同样具有天周期性的特点。利用前4阶EOF基函数和前9项球谐基函数重构的温度修正量校准Jacchia-Roberts模式,校准后的模式密度偏差分别下降了9.06%与5.37%,表明EOF分解方法与传统球谐分析方法相比,能够更有效地修正温度参数,改进模式精度。     

三结太阳电池高能电子损伤模拟及仿真分析

利用wx AMPS软件构建了高效Ga In P/Ga As/Ge太阳电池的中电池模型,并对电池抗辐照性能进行模拟研究。模拟发现,当辐照缺陷密度较小时,缺陷对中电池的电性能影响较小;当缺陷密度较大时,电性能的下降与电子注量值的对数成正比。计算电池的I-V和量子效率谱(QE曲线)可知,电池电性能的下降直接对应于量子效率的下降、饱和暗电流的增强以及并联电阻的衰降。模拟结果与试验结果的对比显示,在各子电池均匀损伤的假定下,1 Me V电子辐照的缺陷引入率约为0.81。     

基于慢特征密度聚类的气路异常检测方法

在结合核技巧、慢特征分析算法与密度聚类方法的基础上,提出了基于混合核慢特征分析和密度聚类的慢特征密度聚类算法,实现了基于民航发动机气路参数原始值的异常检测。核技巧的引入克服了慢特征分析法处理复杂数据时可能存在的维度爆炸问题,充分利用不同核函数的特点和慢特征分析的优势从气路参数原始值中提取出随时间变化最缓慢的特征作为密度聚类算法的输入,最终筛选出异常值。经实验对比发现,该方法针对某些异常拥有最好的聚类效果和最低的虚警率,尤其是检测可调放气活门系统异常时虚警数量不到样本总数量的0.5%,是一种有效的方法。      

超声速尾迹-剪切流的混合增强

超声速条件下燃料和空气之间的高效混合是超然冲压发动机技术上的主要挑战。基于大涡模拟和流动稳定性分析,针对超声速尾迹-剪切流动开展了混合增强方法研究。尾迹的存在改变了混合层流动的速度剖面,对流动稳定性产生了重要影响,使混合层由三维最不稳定变为二维最不稳定,最不稳定扰动波频率和增长率增大。基于流动稳定性结果引入扰动的混合增强方式依然有效,根据稳定性结果设计了波纹隔板。数值结果表明：二维波纹壁引入的扰动未能增长,不具备混合强化效果,而三维波纹壁引入的扰动能够快速增长,具有混合强化效果,且波纹壁参数越接近最不稳定扰动波参数,混合强化效果越明显。     

Analysis on Potential Conflict Frequency of Intersected Air Routes in Terminal Airspace Design

In order to obtain accurate conflict risks in terminal airspace design, the concept and calculation model of potential conflict frequency for intersected routes are proposed. Conflict frequency is represented by the product of horizontal conflict frequency and vertical conflict probability. The horizontal conflict frequency is derived from the probability density distribution of conflicts in a period of time. Based on the recorded radar trajectory data, the concept and model of ROUTE distance are proposed, and the probability density function of aircraft height at a specified ROUTE distance is deduced by kernel density estimation. Furthermore, vertical conflict probability and its horizontal distribution are achieved. Examples of three intersected arrival and departure route design schemes are studied. Compared with scheme 1, the conflict frequency values of the other two improved schemes decrease to 53 % and 24%, respectively. The results show that the model can quantify potential conflict frequency of intersec ted routes.     

玉树地震前的电离层异常现象分析

分析了玉树地震前地基电离层探测临界频率、GPS TEC和卫星探测原位等离子体参量等多个参数的扰动变化信息, 研究了不同高度异常变化的时空关联性. 分析发现, 在地震前一天的4月13日, 多个电离层参量出现同步扰动异常, 电离层临界频率f₀F₂异常相对滑动中值增大40%, 异常空间上存在从震中东南向西南漂移的特性; GPS TEC异常增强15TECU (1TECU=1016m-2)左右, 分布于震中南部经度15°范围内, 且有明显的磁共轭效应; DEMETER观测的原位氧离子密度N_i(O+) 4月13日为1-4月中最强的一天, 异常分布偏向赤道区, 但仅局限在30°-50°左右的经度范围内. 综合三个参量的异常特征发现, 无论是空间的局地性还是时间上的密切关联均反映这次电离层扰动可能与玉树地震孕育有关. 结合其他观测信息, 进一步探讨了这次地震孕育过程的地震电离层耦合机理.      

Assessment of precision in ionospheric electron density profiles retrieved by GPS radio occultations

The Constellation Observing System for Meteorology Ionosphere and Climate (COSMIC) is a six satellite radio occultation mission that was launched in April 2006. The close proximity of these satellites during some months after launch provides a unique opportunity to evaluate the precision of Global Positioning System (GPS) radio occultation (RO) retrievals of ionospheric electron density from nearly collocated and simultaneous observations. RO data from 30 consecutive days during July and August 2006 are divided into ten groups in terms of daytime or nighttime and latitude. In all cases, the best precision values (about 1%) are found at the F peak height and they slightly degrade upwards. For all daytime groups, it is seen that electron density profiles above about 120 km height exhibit a substantial improvement in precision. Nighttime groups are rather diverse: in particular, the precision becomes better than 10% above different levels between 120 and 200 km height. Our overall results show that up to 100–200 km (depending on each group), the uncertainty associated with the precision is in the order of the measured electron density values. Even worse, the retrieved values tend sometimes to be negative. Although we cannot rely directly on electron density values at these altitudes, the shape of the profiles could be indicative of some ionospheric features (e.g. waves and sporadic E layers). Above 200 km, the profiles of precision are qualitatively quite independent from daytime or latitude. From all the nearly collocated pairs studied, only 49 exhibited a difference between line of sight angles of both RO at the F peak height larger than 10°. After analyzing them we find no clear indications of a significant representativeness error in electron density profiles due to the spherical assumption above 120 km height. Differences in precision between setting and rising GPS RO may be attributed to the modification of the processing algorithms applied to rising cases during the initial period of the COSMIC mission.     

Intra-annual variations of the thermospheric density at 400 km altitude from 1996 to 2006

We investigate the intra-annual variations of globally averaged thermospheric density at 400 km altitude from 1996 to 2006 by using Artificial Neural Network Method (ANNM). The results indicate that thermospheric density is governed by solar activity, and the absolute error of our model is 13.67%, less than NRLMSISE-00 model. Fourier representation can catch the intra-annual variations more accurately than NRLMSISE-00 model and JB2008 model especially during 2002. We find that the Autumn maximum is slightly greater than Spring maximum during solar minimum, while the reverse is correct during solar maximum. There is a strong linear relation between solar activity and the amplitude of annual/semiannual variations, and the correlation coefficients are 0.9534 and 0.9424, respectively. Moreover, the amplitude ratio of the annual to semiannual variation is about 1.3 averaged, and changes in different years, but it has little relation with solar activity. Besides that, the amplitude of annual variation is larger than semiannual variation during 1996 and 2006 except 1998 and 2000. The relative error of NRLMSISE-00 model is 14.95%, decreasing to 12.49% after revising, and the correlation coefficients between this empirical model and its improved results and the observation are 0.8185 and 0.9210, respectively. Finally, we suggest the revised version of MSIS series of model should use the Fourier representation to express the intra-annual variations.