太阳风与火星的相互作用

考虑太阳风动压与火星大气中的粒子热压与磁压之和平衡,建立了火星磁层顶形成的理论模型,结合卫星观测数据,对子午面内向日侧火星磁层顶位形进行数值计算和分析,研究了火星磁层顶位形及其与太阳风动压之间的变化关系。结果认为,火星磁层顶位形与地球磁层顶相似;太阳风动压越大,火星磁层顶越靠近火星; 反之,越远离火星。这些结果,对于了解火星感应磁层形成的物理机制有着重要科学意义。     

二维磁流变液的动力学特性

采用朗之万分子动力学,数值模拟研究了二维磁流变液系统的动力学特性.模拟结果表明,磁场会使系统出现链状结构,且随着磁场强度的增加,短链增长,束链出现,与实验结果一致;最大静摩擦力随着磁场强度的增加而减小,但随着无序点钉扎强度的增加而增大.此外,随着外加驱动力的提高,运动系统的链状结构更加明显,束链增多,表明粒子之间的关联会随着外加驱动力的增加而增强.点钉扎无序会破链状结构,破坏程度随着点钉扎强度的增加而增强.     

能量旁路组合发动机磁流体发电通道数值模拟

利用简化的一维低磁雷诺数下磁流体动力学方程组,对理想分段法拉第型MHD发电通道开展了数值模拟研究,分析了电磁参数和通道几何参数的变化对MHD发电通道性能的影响。结果表明:MHD发电通道能够有效减小出口气流速度,降低总温,并提取出能量,但由于电磁作用的不可逆效应以及焦耳热的产生总压有所损失。磁场强度B、电导率σ的大小,反映了通道内电磁作用强度。适度扩张型通道能够抑制出口气流速度、静温和总温,并增强电磁作用效果。要使通道出口速度减小,总温和总压降低,能量提取率增加,可以增大磁场强度B或电导率σ;反之则反向调节。     

磁层亚暴过程中高速流分布

采用实际的磁尾位型,利用数值模拟方法研究磁层亚暴过程中高速流分布。结果表明垂直磁场的高速流主要分布在电流片内,范围在|Z|<0.25RE;平行磁场高速流分布区域在两个区域较大,一个是距离地球较近的磁场较强的区域,另一个是距离等离子体片较近磁场较强的区域。     

J-TEXT装置上的三维磁场分析研究

为了解决二维磁场位形的局限性,对三维磁场位形的研究势在必行。基于J-TEXT平衡参数,利用VMEC程序求解得到J-TEXT装置的三维磁场位形。此外,分析了等离子体电流、压强对磁场位形的影响,论证了VMEC程序应用在J-TEXT上的可行性。结果表明,VMEC程序能够初步满足J-TEXT装置的三维磁场位形研究要求,为后续装置三维磁场位形优化提供理论和工程借鉴意义。通过比较不同的等离子体电流,压强剖面对三维磁场的计算结果,表明了等离子体电流能够改变极向磁场强度,增大压强剖面使等离子体环状膨胀,磁轴外移。     

永磁体作用下电阻点焊熔核中的电磁场分布规律

采用数值模拟方法研究了外加永磁体磁场作用下,电阻点焊熔核内的外部磁场、感应磁场及复合磁场强度及其磁场力的分布规律,并对熔化金属的流体流动模式进行了定性分析.结果表明,在外加磁场作用下,点焊熔核内的复合磁场分布以感应磁场为主导,从熔核中心至边缘逐渐增强,其径向磁感应强度分量随着永磁体工作距离增加而逐渐减小.熔核内同时存在由感应磁场生成的位于电极轴对称平面内的磁场力,以及由外加磁场引起的垂直于该平面的磁场力.在该正交磁场力的作用下,熔核内的熔化金属在电极轴对称平面及垂直于该平面的圆周方向同时进行高速流动,并呈现出沿熔核直径方向向外冲击的趋势.     

纳米带中涡旋畴壁在磁场驱动下的振荡行为

利用微磁学模拟软件(OOMMF),对坡莫合金纳米带中涡旋畴壁在略高于Walker极限的磁场驱动下的动力学行为进行模拟,分析外磁场强度、纳米带尺寸及自旋极化电流对畴壁振荡频率的影响。结果表明,纳米带中涡旋畴壁的振荡频率随外磁场强度的增大而增加,随着纳米带宽度的增加呈先增加后减小再增大最后基本保持不变的趋势;外加与磁场方向相反的平衡电流,虽然不改变畴壁振荡频率随外磁场强度和纳米带宽度的变化规律,但能起到减小畴壁振荡频率的作用,且平衡电流随外磁场强度和纳米带宽度的变化趋势与畴壁振荡频率基本相反,而其随着阻尼系数的增大而线性增加。     

磁层亚暴过程中的磁岛合并特征

采用实际的磁尾位型,利用数值模拟研究地球近地磁尾磁层亚暴过程中的磁岛合并过程,选取了磁尾电流片中三个测量点,分析了电流、磁场、等离子体密度以及速度随时间的变化规律,合理的解释磁层亚暴过程中的观测现象。     

Ni铁磁粒子熵和热容量的影响因素分析

应用统计物理和固体理论,推导了外磁场中镍铁磁粒子的熵、热容量等热力学函数,并利用Mathematica软件进行了数值计算．结果表明：镍铁磁粒子的磁矩与外磁场相互作用引起的熵随温度升高而减小,随外磁场增大而增大;其热容量随温度的升高而增大,随外磁场强度的增大而减小;晶格振动和表面自由能引起的熵和热容量均随温度的升高而增大;温度较低时变化趋势更为显著．     

磁流体条件下气动热特性研究

运用一种适用于高马赫数、低雷诺数流动条件下的磁流体力学(MHD)计算方法研究气动力/热特性.采用经典Hartmann流动验证计算方法的有效性和准确性,通过布置磁场的分布形式、改变磁场强度研究磁场对磁流体流动的影响,包括对激波的控制作用及对壁面压力和热流密度的影响,进而得到磁流体条件下的气动热加热特性.通过研究,得到以下结论:磁场对流动的影响主要通过无量纲互涉参数体现,给定来流条件的情况下,通过提高电导率或增强磁感应强度都可以起到增强磁场效应的效果;磁场对流场作用主要表现为磁阻滞效果,引入磁场后流场变化更为平缓,随着机体内磁场强度增大,激波的脱体位置不断前移、强度逐渐变弱,飞行器表面压力不断升高、热流逐渐下降.     

Dependence of magnetic field just inside the magnetopause on subsolar standoff distance: Global MHD results

The subsolar magnetopause is the boundary between the solar wind and the Earth’s magnetosphere,where reduced solar wind dynamic pressure is equal to the magnetic pressure of the Earth’s outer magnetosphere.We use a global magnetohydrodynamic (MHD)model to estimate the ratio f of the compressed magnetic field just inside the subsolar magnetopause to the purely dipolar magnetic field.We also compare our numerical results to a similar work by Shue,which used Time History of Events and Macroscale Interactions during Substorms(THEMIS)data.Our results show that the ratio f is linearly proportional to the subsolar magnetopause standoff distance(r0)for both the northward and southward interplanetary magnetic field,properties consistent with Shue but with a smaller proportionality constant.However,previous theoretical studies show that f is nearly independent of the subsolar standoff distance.The global model results also show that f is smaller for the southward Interplanetary Magnetic Field(IMF)under the same r0,and that the proportionality constant for the southward IMF is larger than that for the northward IMF.Both conclusions agree with statistical results from observations by Shue.     

Comparison of a new model with previous models for the low-latitude magnetopause size and shape

In this study, the advantages and the limitations of previous low-latitude magnetopause empirical models are discussed. In order to overcome their limitations and inherit their advantages, a new continuous function for the influence of the interplanetary magnetic field (IMF) Bz on the magnetopause, the Shue model function and the 613 low-latitude magnetopause crossings are used to construct a new low-latitude magnetopause model parameterized by the solar wind dynamic pressure (Dp) and IMF Bz. In comparison ...     

Simulation of the dawn-dusk magnetosheath asymmetry under quasi-steady states

The dawn-dusk asymmetry of the magnetosheath under quasi-steady states has been studied by using a newly developed 3D MHD magnetosphere simulation model. The results show that the dawn-dusk asymmetry is substantial because of the Parker spiral IMF. It is found that the dawn-dusk magnetosheath thickness asymmetry is the effect of different shock conditions. The plasma density and flux asymmetry are mainly caused by the different thickness of the dawn-dusk magnetosheath, and the magnetic reconnection on the magnetopause has no significant effects. It is also showed that the Plasma Depletion Layer in front of the dayside magnetopause can cause duskward plasma flow, and the total plasma flux on the dusk side will be higher.     

基于经验模态分解的自适应噪声对消方法

针对飞行器试验中单通道遥测信号频率内容丰富、降噪困难的问题,提出了一种基于经验模态分解的自适应噪声对消方法。将信号利用经验模态分解(Empirical mode decomposition, EMD)方法分解为一系列本征模态函数(Intrinsic Mode Function,IMF),将第一阶IMF作为参考噪声,并将第二阶以后的IMF分量累加求和,作为待降噪信号,在此基础上利用自适应噪声对消系统完成降噪。该方法克服了直接将高阶IMF作为噪声消除后在降噪和细节信息损失之间的矛盾性问题,可以最大程度保护信号细节信息不受损失的情况下实现良好的降噪效果。计算机仿真和某次飞行器试验实测数据处理结果证明了这一方法的有效性。     

Simulation of mode conversion at the magnetopause

Two-dimensional(2-D)and three-dimensional(3-D)hybrid simulations are carried out for mode conversion from fast mode compressional wave to kinetic Alfvn waves(KAWs)at the inhomogeneous magnetopause boundary.For cases in which the incident fast wave propagates in the xz plane,with the magnetopause normal along x and the background magnetic field pointing along z,the 2-D (xz)simulation shows that KAWs with large wave number kxρi～1 are generated near the Alfve′n resonance surface,whereρi is the ion Larmor radius.Several nonlinear wave properties are manifest in the mode conversion process.Harmonics of the driver frequency are generated.As a result of nonlinear wave interaction,the mode conversion region and its spectral width are broadened.In the 3-D simulation,after this first stage of the mode conversion to KAWs with large kx,a subsequent generation of KAW modes of finite ky is observed in the later stage,through a nonlinear parametric decay process.Since the nonlinear cascade to ky can lead to massive transport at the magnetopause,the simulation results provide an effective transport mechanism at the plasma boundaries in space as well as laboratory plasmas.     

Observation and simulation of flux rope structures at the dayside magnetopause

The signatures of flux ropes with obvious core magnetic field are detected by Cluster Ⅱ at the dayside magnetopause during 11:00--11:15 UT on Mar. 2, 2001. The similar characteristics can be found from the magnetic fiel dvariations recorded by the four spacecrafts (Cluster Ⅱ C1--C4). All the three (-/ ) bipolar signatures in the BN component are accompanied with enhancements of BM and magnetic field strength B in the boundary normal coordinates (LMN coordinates). A MHD simulation with two dimensions and three components is performed to explore the reconnection process driven by the incoming flow of solar wind at the dayside magnetopause. The numerical results can illustrate the recurrent formation of magnetic structures with a core magnetic field. The time history of the magnetic field B and three components Bx, By and Bz at a given point of the current sheet can reproduce the observational features of the events mentioned above.     

Single-fluid 2D magnetohydrodynamic simulation of solar wind structure in comparison to ulysses observations

Two dimensional Magnetohydrodynamic (MHD) equations with and without the momentum addition respectively have been used to simulate the solar wind structure on the meridian plane. The results show that far away from the sun it isn't solar magnetic field that induces the cncave solar wind speed. Instead, there may be the fast speed streamer driven by the momentum addition and an interface between high and low speed streamers. The interaction between high and low speed streamers causes the sharp division. Foundation item: Supported by the National Natural Science Foundation of China (4999045) Biography: Deng Ling-yun (1976-), female, Master candidate, research direction: solar-terrestrial physics.     

基于经验模态分解的煤矿设备温度预测

煤矿设备出现故障时,设备温度会迅速上升,表现出非线性和非平稳性的特点。为了较准确地预测温度异常,采用了基于经验模态分解（EMD）的神经网络方法对设备温度进行预测。该方法首先采用经验模态分解算法对设备温度时间序列进行分解,得到若干个平稳性较好的本征模态函数（IMF）分量和一个剩余量,然后分别对各分量及剩余量进行神经网络预测。仿真结果表明,基于EMD的神经网络预测方法比单一神经网络预测方法,预测精度更高,对于温度异常预测更有效。     

光束通过棱镜的变换矩阵

利用光束斜入射到界面的变换矩阵，推导光束通过棱镜时在子午面和弧矢面的变换矩阵，并得出光束通过棱镜时所产生的像散与光束入射的位置、入射角及棱镜顶角相关的结论。     

基于改进信息熵和LSTM网络的轴承故障诊断

针对传统的时频域故障诊断方法无法对故障实现自适应识别和分类,且准确率较低的问题,提出了一种基于改进信息熵(IIE)的长短时记忆网络(LSTM)方法。首先对原始信号分别进行集合经验模态分解(EEMD)和变分模态分解(VMD);将包含故障信息的所有本征模式分量(IMF)进行信息熵的求取;通过信息熵反应IMF的信息量和峭度指标对描述冲击成分的优势改进信息熵,构成特征向量;最后结合LSTM处理非线性数据的优势,利用组合特征训练LSTM网络建立诊断模型。实验结果表明:该方法能准确、高效地识别多种故障,准确率要比单一的EEMD-LSTM、VMD-LSTM、人工神经网络等传统方法更高。