基于磁检测的AGV导引新方法

利用磁阻传感器作为磁导引路径的检测元件,实现了准确的磁路径定位,在此基础上实现了磁导引。详细介绍了磁检测方法、导引原理以及控制方案。当AGV产生一定范围的位置偏差时（水平偏移不大于±5cm,角度偏转不大于±25°）,该方法可以准确的检测并计算出位置偏差并进行相应控制。实验结果表明,该磁导引方式定位准确且易于实现。     

一种重力卫星质心在轨标定算法

针对重力卫星质心在轨标定问题,提出了一种将预测滤波与卡尔曼滤波相结合的标定算法。该算法首先利用磁力矩器产生一个明显大于干扰力矩的周期性力矩作用于卫星上,然后利用陀螺数据实现了卫星角加速度的预测滤波估计,并通过静电加速度计信息设计卡尔曼滤波器,实现卫星质心的标定;最后进行了数学仿真,仿真结果表明该算法针对卫星的角加速度及质心位置能够实时估计,三轴最佳标定精度分别为[0.0628 0.0324 0.0414]mm,实现了卫星质心较为精确的标定。     

Alfven波在微电离大气中的衰减特性研究

利用简单的偶极子地磁场模型以及大气电子密度和电导率模式, 分析地面产生的磁扰动以Alfven波的模式传播到近地空间区域. 这种地面的磁扰动可能干扰近地空间卫星对空间磁扰动的观测. 通过对地面磁扰动Alfven波模式1000 km高度内的衰减情况进行模拟, 认为在近地空间采用地磁偶极子模型是合理的. 由于衰减随扰动频率的增大而急剧增强, 分析还得到了近地卫星能够探测到地面磁扰动的最大频率. 计算结果表明, Alfven波的衰减主要集中在高度50 km以下, 这个区域内的大气电导率极其微弱, 使Alfven波的传播受到极大衰减. 0.4 Hz以下的Alfven波沿磁力线传播到1000 km高度后衰减结为原来扰动幅度的千分之一, 因此频率在0.4 Hz以下的Alfven波可能会干扰低轨卫星探测磁场脉动.      

太阳风中小尺度磁通量管边界重联的统计研究

通过对WIND卫星1995—2005年的数据,利用程序筛选及人工识别两种不同方法确定的小尺度磁通量管进行比较,发现程序筛选法中41%的小尺度磁通量管有边界重联现象,与人工识别法确定的小尺度磁通量管的统计结果接近;通过人工识别和程序筛选两种方法确定的小尺度磁通量管的边界重联特征,包括磁场剪切角、磁场强度以及重联耗散区的持续时间等,也具有相同的统计趋势.结果表明,两种方法确定的小尺度磁通量管在重联特性上没有本质区别,因此采用这两种方法得到的数据作为样本来统计小尺度磁通量管前后边界重联事件.本文共确定了71个重联事件,统计结果显示有50个(70%)重联耗散区磁场的减小超过20%,47个(66%)磁场剪切角大于90°;多数重联事件的磁场剪切角大于90°,表明小尺度磁通量管边界中主要发生的是反平行重联.将小尺度磁通量管的前后边界重联分开进行统计,结果显示其前后边界重联的特征是相似的,与磁云前后边界存在差异的性质不同,这意味着太阳风中的小尺度磁通量管并不具有磁云这种大尺度磁通量管的膨胀特征.     

2010年4月地球同步轨道相对论电子增强事件分析

为研究2010年4月地球同步轨道相对论电子通量异常增强事件的原因, 选取了2004-2010年之间高速太阳风下7个类似事件进行对比分析. 探讨了多种可能导致此次异常事件的太阳风和地磁条件. 结果表明, 较弱的磁暴使得相对论电子高通量区域更接近同步轨道, 此外, 哨声波加速很可能在2010年4月地球同步轨道相对论电子通量异常增强事件中起到重要作用. 磁暴强度与种子电子的注入深度密切相关, 表现为Dst指数曲线的形态与能量为30～100keV的电子高通量区域的下边缘高度吻合. 能量为30～100keV电子的注入深度影响了能量大于300keV的电子出现的磁层区域. 此事件中, 由于磁暴相对较弱, 种子电子向内磁层注入的深度较浅, 更靠近同步轨道区域, 这使得相对论电子大量出现的区域也靠近同步轨道, 最终导致同步轨道相对论电子通量异常增强. 另外, 2010年4月地球同步轨道相对论电子通量异常增强事件中, 高强度的亚暴提供了充足的种子电子并加强了波粒相互作用, 这也是相对论电子增强的必要条件.      

Numerical investigation of the influence of large turbulence scales on the parallel and perpendicular transport of cosmic rays

In recent analytical investigations it has been demonstrated that the turbulence behavior at large scales has a very strong influence on the perpendicular diffusion coefficient of charged particles. In the present paper we use computer simulations to investigate numerically cross field transport and particle propagation along the mean magnetic field for different turbulence models at large scales. Our results are compared with quasilinear theory and nonlinear diffusion theories. We show that for different forms of the turbulence spectrum at large scales, the perpendicular mean free paths obtained numerically are in agreement with recent predictions made by analytical theory. It is also shown that the parallel diffusion coefficient contains always a strong nonlinear contribution which is, however, independent of the assumed spectrum at large scales.     

抗磁性物质磁悬浮方法在空间生物学与生物技术中的应用

失重是特定空间运动条件下的重要环境物理特征之一, 一般以微重力环境来表示. 几十年来人类利用空间失重环境进行了多学科领域的科学研究与探索. 由于真实空间失重环境下科学实验机会稀少, 人类为研究空间失重环境或效应, 开发了多种地基的空间模拟实验技术方法. 然而, 对于空间生物学和空间生物技术研究而言, 已有的各种模拟实验技术手段在原理上和应用上均存在一定的局限性. 本文介绍了抗磁性物质在大梯度强磁场中的悬浮现象, 及将其用于模拟空间失重环境的方法与原理;简述了近年来利用抗磁性物质悬浮方法进行生物大分子晶体生长、分子细胞生物学及整体生物学等方面研究与应用的进展.      

Drag balance Cubesat attitude motion effects on in-situ thermosphere density measurements

The dynamics of Cubesats carrying a drag balance instrument (DBI) for in situ atmosphere density measurements is analyzed. Atmospheric drag force is measured by the displacement of two light plates exposed to the incoming particle flow. This system is well suited for a distributed sensor network in orbit, to get simultaneous in situ local (non orbit averaged) measurements in multiple positions and orbit heights, contributing to the development and validation of global atmosphere models. The implementation of the DBI leads to orbit normal pointing spinning two body system. The use of a spin-magnetic attitude control system is suggested, based only on magnetometer readings, contributing to making the system simple, inexpensive, and reliable. It is shown, by an averaging technique, that this system provides for orbit normal spin axis pointing. The effect of the coupling between the attitude dynamics and the DBI is evaluated, analyzing its frequency content and showing that no frequency components arise, affecting the DBI performance. The analysis is confirmed by Monte Carlo numerical simulation results.     

Observations of Extended Radio Emission in Clusters

We review observations of extended regions of radio emission in clusters; these include diffuse emission in ‘relics’, and the large central regions commonly referred to as ‘halos’. The spectral observations, as well as Faraday rotation measurements of background and cluster radio sources, provide the main evidence for large-scale intracluster magnetic fields and significant densities of relativistic electrons. Implications from these observations on acceleration mechanisms of these electrons are reviewed, including turbulent and shock acceleration, and also the origin of some of the electrons in collisions of relativistic protons by ambient protons in the (thermal) gas. Improved knowledge of non-thermal phenomena in clusters requires more extensive and detailed radio measurements; we briefly review prospects for future observations.     

The Geophysics of Mercury: Current Status and Anticipated Insights from the MESSENGER Mission

Current geophysical knowledge of the planet Mercury is based upon observations from ground-based astronomy and flybys of the Mariner 10 spacecraft, along with theoretical and computational studies. Mercury has the highest uncompressed density of the terrestrial planets and by implication has a metallic core with a radius approximately 75% of the planetary radius. Mercury’s spin rate is stably locked at 1.5 times the orbital mean motion. Capture into this state is the natural result of tidal evolution if this is the only dissipative process affecting the spin, but the capture probability is enhanced if Mercury’s core were molten at the time of capture. The discovery of Mercury’s magnetic field by Mariner 10 suggests the possibility that the core is partially molten to the present, a result that is surprising given the planet’s size and a surface crater density indicative of early cessation of significant volcanic activity. A present-day liquid outer core within Mercury would require either a core sulfur content of at least several weight percent or an unusual history of heat loss from the planet’s core and silicate fraction. A crustal remanent contribution to Mercury’s observed magnetic field cannot be ruled out on the basis of current knowledge. Measurements from the MESSENGER orbiter, in combination with continued ground-based observations, hold the promise of setting on a firmer basis our understanding of the structure and evolution of Mercury’s interior and the relationship of that evolution to the planet’s geological history.