磁暴对赤道地区L波段电离层闪烁的影响研究

利用赤道地区Vamimo站闪烁数据, 选取两次典型大磁暴时段重点分析, 对比磁暴发生前、发生时以及发生后连续几天电离层幅度闪烁强度和发生率的变化, 引入瑞利elax-elax泰勒不稳定性(Rayleigh-Taylor, R-T不稳定性)线性增长率γ₀, 对磁暴影响闪烁的机制进行初步探讨. 结果表明, 磁暴可能触发闪烁发生, 也可能抑制闪烁发生, 这既与观测季节有关, 也与磁暴不同发展阶段的地方时有关. 触发发生于闪烁少发季节磁暴主相所在的午夜至黎明时段, 可能是磁层穿透电离层的东向电场所致; 抑制发生于闪烁多发季节磁暴恢复相所在的午夜前时段, 可能是西向电场作用的结果. 磁暴发生时的电场变化可能是抑制或触发闪烁的主导因素, 但仍需进一步分析研究.      

带扰流柱内冷通道对表面气膜冷却特性的影响

为了讨论内冷通道结构对表面气膜冷却特性的影响,通过数值模拟的方法,计算研究不同结构下,冷气流过带有扰流柱内冷通道对表面气膜冷却特性的影响,并研究冷气通道与燃气掺混后的冷却效果;采用六种不同结构的扰流柱与气膜孔排列方式,计算中吹风比的范围为0．1〈M〈2．0。结果表明：冷气通道内的扰流柱对进入气膜孔的冷气起到稳定作用,比冷气通道内不加扰流柱的气膜冷却效果好,而且扰流柱与气膜孔不同的排列方式对气膜冷却效果有显著影响,因此选择合适的排列方式有利于气膜冷却。     

发动机高压两级涡轮盘联合低循环疲劳寿命试验

以某型发动机高压两级涡轮盘为研究对象,通过有限元计算得到试验载荷系数,组装和调试了全尺寸联合试验件,完成了低循环疲劳试验,得到了以传动臂销钉孔为定寿部位的两级涡轮盘低循环疲劳寿命。两级涡轮盘联合低循环疲劳试验在国内尚属首次,相对于单盘低循环疲劳试验,更加符合发动机实际工作状态,将传动臂销钉孔作为两级涡轮盘的定寿部位更为合理。该联合试验为外场涡轮盘重新定寿提供了依据。     

一种利用剩磁标定的星光/磁测备份自主导航方法

针对空间机动平台GNSS导航系统易受干扰的缺陷,提出一种基于剩磁标定的磁测/星光备份的自主导航方案。当GNSS信号完好时,利用GNSS高精度测量信息和磁强计/星敏带剩磁干扰的联合测量信息不仅可实时估计出机动平台导航参数,同时准确标定出运行环境的剩余磁场强度;当GNSS信号受干扰中断时,在剩磁准确标定的基础上启用磁场/星光备份自主导航方案完成机动平台的导航参数实时估计。由仿真结果可知,当GNSS信号正常时该导航方案具备较高的剩磁标定精度,三轴标定误差为0.026nT,0.293nT,0.107nT;而当GNSS信号受干扰时,备份导航方案三轴位置估计误差为87.3m,172.5m,65.2m,三轴速度估计误差为0.78m/s,0.86m/s, 1.04m/s。 仿真结果表明该方案具备较强的可行性。     

Global Hybrid Simulation of Magnetic Reconnection in the Magnetosheath

A three-dimensional (3-D) global hybrid simulation is carried out for the generation and structure of magnetic reconnection in the magnetosheath due to interaction of an interplanetary Tangential Discontinuity (TD) with the bow shock and magnetosphere. Runs are performed for solar wind TDs possessing different initial half-widths. As the TD propagates through the bow shock toward the magnetopause, it is greatly narrowed by a two-step compression processes, a "shock compression' followed by a subsequent ``convective compression'. In cases with a relatively thin solar wind TD, 3-D patchy reconnection is initiated in the transmitted TD, forming magnetosheath flux ropes. Multiple components of ion particles are present in the velocity distribution in the magnetosheath merging, accompanied by ion heating. For cases with a relatively wide initial TD, a dominant single X-line appears in the subsolar magnetosheath after the transmitted TD is narrowed. A shock analysis is performed for the detailed structure of magnetic reconnection in the magnetosheath. Rotational Discontinuity (RD)/Time-Dependent Intermediate Shock (TDIS) are found to dominate the reconnection layer, which and some weak slow shocks are responsible for the ion heating and acceleration.      

Observations of Magnetic Reconnection in the Magnetotail Associated With Substorms

Magnetic reconnection is one of the most important, dynamic phenomena in the magnetotail in terms of magnetic field line configuration change and energy release. It is believed to occur in the distant magnetotail mainly during southward interplanetary magnetic field periods and in the near-Earth magnetotail in association with substorms. In the present paper, we discuss several important issues concerning magnetic reconnection in the magnetotail associated with substorms, such as reconnection signatures, location, timing, spatial scale, and behavior, from the macroscopic, observational point of view.      

自适应滤波在磁暴期间地磁导航中的应用

对磁暴期间巡航导弹巡航段的地磁导航问题进行了讨论。针对地磁导航在磁暴期间常规卡尔曼滤波容易发散的问题,提出了一种基于Sage\|Husa自适应卡尔曼滤波的地磁导航算法。算法根据新息的变化自适应调整测量噪声矩阵,消除了磁暴影响,提高了滤波稳定性。仿真表明在选择合适的遗忘因子基础上,即使在磁暴最剧烈的时间段,采用自适应卡尔曼滤波仍能保证一定的精度,定位精度在200m以内,满足巡航导弹中程制导的精度要求。     

基于BP神经网络的磁悬浮飞轮控制

针对磁悬浮飞轮控制对鲁棒性、低功耗及不平衡振动抑制等要求,提出BP神经网络直接控制方法。设计了两层结构BP神经网络控制器,基于磁轴承电磁力方程推导网络权值更新算法,实现了神经网络的在线训练。仿真表明,控制器权值更新算法对环境变化适应能力强,训练成功率高;BP神经网络控制器具有起浮迅速、抗干扰能力强、功耗低等性能,并具备不平衡振动抑制能力。结果表明BP神经网络控制器满足磁悬浮飞轮控制要求,具有可行性和有效性。     

一种超薄反作用飞轮的大面积磁悬浮结构分析

为提高轴向磁通反作用飞轮的轴向刚度和寿命,结合轴向磁通飞轮的结构,提出一种超薄、大面积磁悬浮的反作用飞轮。重点分析该飞轮的大面积磁悬浮结构,从磁环的宽度、磁环的充磁方向、磁环间距、铁芯厚度和磁悬浮刚度五个方面展开研究。通过有限元仿真可以发现：随磁环宽度的增加,定子对转子的斥力是先增大后减小;定子内外环磁化方向相反时比相同时能得到更大的斥力;在内外环磁化方向相反时,内外环磁钢间距越小,定子对转子斥力越大;磁悬浮部分铁芯厚度的减小对定转子间的斥力的影响极其有限,但对降低飞轮重量具有重要意义;磁悬浮的刚度与转子偏离中心的距离近似成正比。     

Magnetic reconnection on the Sun: ESPD Senior Prize Lecture

Magnetic reconnection is a fundamental process for changing the magnetic topology and converting magnetic energy into other forms on the Sun, such as heat, flow energy and fast particle energy. In two dimensions it is fairly well understood, although some aspects still need to be developed. In three dimensions, it behaves very differently and a substantial body of theory and numerical experiment has now been built up, including reconnection at null points, separators and quasi-separators.Some aspects of solar flares can be understood with 2D reconnection models, but other aspects such as the shapes of flare ribbons, the acceleration of particles and the creation of twist in erupting flux ropes need a 3D understanding. A paradigm shift in our understanding of coronal heating by reconnection has been stimulated by dramatic new observations of photospheric flux cancellation from SUNRISE and from SST together with the realisation that it may well be driving nanoflare heating events and possibly campfires.