十字形磁梯度张量结构在多磁偶极子测量中的误差与修正方法

磁场全张量探测技术在多磁源反演中有着重要意义。十字形磁梯度张量结构因其计算简单、精度高等特点被广泛采用,但其在多磁源反演中的全方位误差分析和修正方法有待完善。文章研究多磁偶极子分辨的问题,分析十字形计算结构和误差来源;结果表明磁力仪的精度、整体结构、背景环境和基线选取都会造成误差,甚至导致错误;最后给出修正方法和建议,同时提出可行的扫描方法。     

基于全张量磁场梯度的磁偶极子定位及误差分析

为了对磁偶极子进行高精度的磁性定位,文章从磁偶极子模型出发,推导出磁偶极子的空间坐标与其产生的磁场及磁场梯度之间的关系式;针对模型及关系式,设计了一种全张量磁场梯度传感器,能够一次测量出精确定位所需的9个磁场梯度值和3个磁场强度值;对比仿真结果和实验结果,发现二者具有较好的一致性,证明了该理论模型的有效性。对于磁偶极子,用半径为0.05 m的梯度传感器对磁矩为2 A·m~2的磁偶极子进行定位测量,在0.5~1 m距离内定位误差不大于10%。文章还对定位测量误差的原因进行了分析,包括梯度测量基线距离及传感器半径对定位误差的影响。     

基于双星编队SAR三轨法差分干涉技术的基线设计

将单星重复轨道三轨法差分干涉扩展到双星编队,对正侧视下合成孔径雷达差分干涉(DInSAR)技术的基线设计进行了研究。在测量坐标系中,将位于主星距离高度平面内的简化基线扩展为空间矢量,根据空间几何关系得到正侧视下双星编队SAR三轨差分干涉法的空间基线模型。建立了编队SAR测高程时基线设计公式,以及基线矢量到DInSAR测形变所需基线的转换公式,基于该模型首次从应用角度分析了基线对编队SAR三轨法差分干涉测形变的误差传播特性。给出了基于基线比的基线设计方法:测高程时,基线选择以临界基线为上限,综合考虑测高精度和灵敏度确定基线;测形变时,为降低误差对形变精度的影响,基线比应尽量小(基线比为0.25时编队SAR三轨法DInSAR形变测量精度最高),即地形图像对的垂直有效基线应尽量大,形变图像对的基线应尽量小。用ALOS-2卫星参数进行了仿真计算,所得编队基线和重复轨道基线误差要求分别为毫米级和厘米级。研究对DInSAR系统中基线参数设计有更直观的理论指导意义和实际应用价值。     

嫦娥一号卫星星地时差校正量计算方法研究

影响月球探测卫星星地时差的因素较多，文章介绍了其计算模型，并对其中的模糊距离进行了详细分析。通过对试验数据的分析，运用最小二乘法，分别建立了集中校时量和均匀校时量计算模型。实际结果表明：运用此两种校时模型和方法可以方便有效地控制嫦娥一号卫星的星地时差，并使其在一段时期内保持在5ms范围以内。     

月球探测器定轨误差分量协方差分析

基于测量量的数学模型,推导环月探测器状态矢量的信息阵,建立定轨误差RTN分量的误差方程和协方差矩阵,给出了测距、测速、时延和时延率的测量误差对定轨误差RTN分量影响的数值关系。根据中国探月工程实际轨道测量数据精度和测站／基线分布情况,计算分析了2种环月轨道位置速度误差RTN分量的影响因素和误差水平。利用嫦娥-1、2月球探测器实际定轨结果,验证了分析方法的有效性。该方法对中国探月工程二期任务动力下降初始定轨误差RTN分量计算具有参考意义。     

单航过单平台InSAR基线模型的敏感性分析

从单航过单平台InSAR系统对其自身基线的高精度需求出发,给出了光学测量方案下的基线模型,并针对模型中的各因素及其误差来源,进行了模型的敏感性分析,阐明了测量元素与位置修正矢量的基线矢量的误差传递关系,然后根据误差传递关系找出测量系统的优化安装部位。通过解析推导得出各类误差源在不同条件下对基线精度影响的理论结果,由仿真分析给出了不同安装部位的误差传递系数。通过敏感性分析可由测量环境的输入条件直接获得基线的误差量级,其结果可作为指导测量系统方案设计与精度分配的参考依据。     

分布式小卫星雷达系统误差估计的新方法

相干联合处理小卫星编队雷达接收的地面回波可在获得大的成像测绘带的同时获得较高的方位分辨力，具有非常重要的军事应用前景。然而复杂的分布式小卫星雷达系统误差尤其是三维基线误差和多通道幅相误差，严重影响了联合处理各卫星回波数据的效果，甚至使其失败。针对这一问题，提出了一种新的分布式小卫星系统误差补偿方法，该方法不需要迭代运算，可在基线误差控制在分米数量级的基础上对回波信号的空间导向矢量进行准确估计。计算机仿真验证了方法的有效性。     

20cm离子推力器束流平直度的改进方案

针对20 cm离子推力器(LIPS-200)存在束流平直度较差等问题,分析了提高LIPS-200束流平直度的几种方法,主要包括采用4极磁场、阴极前端增加挡板、改变供气方式和栅极孔径补偿设计等。利用数值方法详细研究了磁场对推力器束流平直度的影响。PIC-MCC方法用于模拟放电室内的等离子体放电过程,粒子模拟的磁场输入利用有限元软件MAXWELL计算得到。计算表明,优化磁路结构后的推力器比基线推力器束流平直度提高了29%,同时放电损耗下降了3%。通过分析可看到,单独优化磁路结构或者将优化磁路结构与其他方法相结合能有效提高LIPS-200的束流平直度。     

深空探测器三程多普勒建模与算法实现

针对高精度深空探测多普勒应用,提出了一种间接使用中心天体、航天器的速度与加速度进行多普勒建模的方法。避免了计算机字长截断误差、星历表插值误差对建模精度的影响。使用该算法对环火星探测器进行了连续1周的多普勒计算,通过常规的距离差分方法检验了算法的正确性,对计算的1小时多普勒数据进行10阶多项式拟合,拟合后数据残差小于0.002 mm/s.分析结果表明该算法计算多普勒结果正确,计算精度较常规距离差分算法在精度上得到1个量级的提升。     

对流层散射传播特性及信号谱特性分析

文章介绍了3种对流层散射传播机制，并对不同参数下的对流层散射链路传输损耗进行了计算。结果表明，参数为5GHz频段和100km的典型散射链路，其传输损耗超过200dB。在广义散射截面模型的基础上建立了对流层散射信号传输函数模型，重点研究了对流层散射信号的延迟功率谱特性；从实际散射链路出发，对不同基线距离下的归一化延迟功率谱进行了计算和分析，结果表明，基线距离越远，则波束宽度越宽，相应的归一化延迟功率谱扩展越宽。     

基于欧拉方法的多磁偶极子分辨技术

文章首次将欧拉反演方法应用于航天器内部多磁偶极子的分辨,通过测量航天器外围磁场及其梯度张量数据,采用欧拉反演算法来计算航天器内部主要磁性部组件的位置和磁矩参数。根据磁场梯度张量数据的测量特点,采取了网格式数据采集方式;然后推导了多点联合反演的欧拉方程组,并提出了一种在所有反演解中快速准确寻找最优解的方法;在此基础上利用遗传算法对反演最优解进行了优化。优化后的分辨结果表明:在小范围、多层次磁源分辨方面,计算出的磁源磁矩参数较为准确,且磁源位置最高分辨率优于0.01m。     

基于磁场梯度张量的航天器内部多磁场源探测技术

基于磁场梯度张量的探测技术具有高分辨率、高精度等优点,是航天器多磁源分辨的有效方法。文章建立了航天器磁场源模型,提出了航天器多磁场源模型拟合方法,利用磁场梯度张量的主不变量的极值确定磁场源个数和水平位置,然后联合欧拉方程计算磁场源深度,完成航天器内部多磁场源仿真与计算,分辨率最高可达0.012 m,满足工程需求。该研究开辟了航天器内部多磁场源目标探测的新途径。     

Low-energy ion fluxes and magnetic field on the inner boundary of the heliosphere

A comparison of temporal profiles of low-energy ion intensity and magnetic field magnitude in different periods of solar activity in the outer heliosphere is carried out using the data of the Voyager 1 and Voyager 2 spacecraft. It is shown that temporal, spectral, and statistical characteristics of particle fluxes and magnetic field in the heliospheric regions before and after the terminal shock in 2002–2008 had similar dynamics in different hemispheres. This similarity allowed one to assume that, in the region of the inner heliospheric boundary, a quasistable spatial structure existed moving together with the terminal shock in accordance with the solar wind pressure, as well as, probably, under the action of the interstellar medium. It was revealed that the spatial dimensions of most details of this structure are less on Voyager 2, which, probably, is due to variation of the solar activity level, difference in latitude of spacecraft disposition, and also the influence of the interstellar magnetic field.     

电磁阀启闭特性非接触测量方法研究

为实现对电磁阀特性进行非接触测量,通过分析电磁阀动作时周围漏磁场的变化,设计了一种新型磁敏感器.该磁敏感器结构简单,操作方便,通过采取合理的抗干扰措施可充分降低旁磁场的影响,提高电磁阀漏磁场测量的可靠性.利用本磁敏感器对实际电磁阀的启、闭特性进行了测量.结果表明,该方法可靠性高,满足电磁阀非接触测量的需要.     

Attitude control system of the first Russian nanosatellite <Emphasis Type="Italic">TNS-0 no. 1</Emphasis>

The results of designing the attitude control system of the first Russian nanosatellite TNS-0 no. 1 providing orientation of its longitudinal axis along the local geomagnetic field induction vector are presented. The system consists of a permanent magnet and two sets of hysteresis rods. The magnetic and geometric parameters of the magnet and rods are calculated. The influence of the permanent magnet field on the hysteresis rods and mutual influence of the rods in the case of compact satellite packaging are analyzed. Examples of calculations of transient processes and steady-state angular satellite motion are presented.     

Ascending flows in the solar atmosphere and formation of the solar wind

Some morphological features of solar magnetic fields in the chromosphere and corona are considered based on studying various observational data. These data are compared to the results of observation of the solar wind and interplanetary magnetic field, as well as to the data on fluxes of solar cosmic rays. New specific features are found in the solar wind structure, and new additional indications of sources of the solar wind are obtained. The properties of the active regions and coronal holes are considered. A model of the ascending stream-like plasma flow is suggested. It flows around the discrete arched magnetic field tubes in the solar atmosphere and stretches them out into interplanetary space.     

Structure of current and plasma in current sheets depending on the conditions of sheet formation

The structure of current sheets created under laboratory conditions is characterized by a large variety, which depends substantially on the conditions under which the sheet if formed. In this work, we present the results of an experimental study of the structure and evolution of current sheets that were formed in magnetic configurations with a singular line of the X type. It has been shown that the change in the transverse magnetic field gradient, the strength of the longitudinal magnetic field, and the mass of the ions in plasma makes it possible to significantly vary the main parameters of the current sheets. This offers the challenges of using laboratory experimental results for analyzing and simulating the cosmophysical processes.     

Fine structure of interplanetary shock fronts from the data of the BMSW instrument of the PLASMA-F experiment

The paper is concerned with studying the thickness of fronts of 38 interplanetary shocks detected by the BMSW instrument, which is a part of the scientific payload of the SPEKTR-R spacecraft, which was launched into a highly elliptical orbit in 2011. The main parameters of the interplanetary shocks have been calculated as follows: the ratio of thermal pressure to magnetic pressure before the front β, the angle between the shock front normal and the undisturbed magnetic field θ_Bn, the ratio of the shock propagation velocity to the magnetosonic velocity in the undisturbed region M_ms, and the shock front velocity relative to the Earth. It has been shown that the front thickness determined from the plasma parameters approximately matches the front thickness obtained from the magnetic field measurements and lies between 0.5 and 5 proton inertial lengths. In some events, the oscillations have been observed (upstream and downstream of the shock) in plasma parameters and in the magnetic field data. The length has been found to be between 0.5 and 6 proton inertial lengths for the preceding oscillations and between 0.5 and 10 proton inertial lengths for the following oscillations. The average value of the proton inertial length is 62 km.