微纳聚合体卫星的对称式重构规划算法

为解决微纳聚合体卫星变构过程中,聚合体各部分之间的动力学耦合导致的卫星整体姿态翻转或紊乱,提出了一种对称式变构规划算法。首先建立了铰链约束下的漂浮基多刚体系统动力学模型,研究了重构过程中各运动模块对本体姿态的影响,提出当每两个运动模块位置与转动方向满足对称性条件时,两者对本体姿态的影响可在一定程度上相互抵消。基于上述理论,在A*算法中引入最优分配度量和对称性判定,设计了并行对称重构规划算法。仿真结果表明,该规划算法可实现重构过程中多模块并行、对称运动,重构过程总步数较少,运动模块对本体姿态的影响小。     

基于磁路法与等效热网络法的航天 永磁同步电机设计与仿真

针对航天永磁同步电机方案初步设计耗时长、过度依赖商业软件的问题,基于磁路法和热网络法,提出了一套方案设计阶段航天永磁同步电机磁热性能快速预估与仿真方法。给出了定子内径、定子外径、铁芯长度、匝数等关键参数的取值准则,建立了包含36个节点集总参数热网络模型,并以端部绕组为例给出了热平衡方程的详细推导过程。通过与成熟商业软件对比,其电磁计算最大误差出现在电流有效值上,偏差值为607%;与样机实测值对比,绕组温升最大误差为73%,满足方案设计阶段预示精度要求,为方案设计阶段航天永磁同步电机快速性能预估提供有力支撑。     

Geomagnetic activity associated with magnetic clouds,magnetic cloud-like structures and interplanetary shocks for the period 1995–2003

Using nine years (1995–2003) of solar wind plasma and magnetic field data, solar sunspot number, and geomagnetic activity data, we investigated the geomagnetic activity associated with magnetic clouds (MCs), magnetic cloud-like structures (MCLs), and interplanetary shock waves. Eighty-two MCs and one hundred and twenty-two MCLs were identified by using solar wind and magnetic field data from the WIND mission, and two hundred and sixty-one interplanetary shocks were identified over the period of 1995–2003 in the vicinity of Earth. It is found that MCs are typically more geoeffective than MCLs or interplanetary shocks. The occurrence frequency of MCs is not well correlated with sunspot number. By contrast, both occurrence frequency of MCLs and sudden storm commencements (SSCs) are well correlated with sunspot number.     

磁悬浮框架飞轮磁轴承技术研究与发展现状

对磁悬浮框架飞轮(MSGFW)和高精度磁轴承研究现状及其未来发展进行了详细阐述。根据转子悬浮力类型，将磁悬浮框架飞轮分为磁阻力构型、洛伦兹力构型和混合力构型，并结合三种构型论述了国内外框架飞轮的发展过程。在此基础上，对球面磁阻力磁轴承和洛伦兹力磁轴承进行了详细介绍，并结合磁路图分析其工作原理，比较了同类磁轴承的优劣。展望了磁悬浮框架飞轮与高精度磁轴承的未来发展方向，指出高动态响应检控共位平动球面磁阻力磁轴承，标准磁悬浮动量球和磁悬浮控制敏感球是磁悬浮框架飞轮的研究重点。     

基于遗传算法的地磁匹配搜索策略

为降低导航成本,提出仅利用磁测计和里程计的地磁场匹配定位方法.为解决搜索空间过大的问题,提出以遗传算法在匹配区域搜索可能路径的方法.该方法以相关性度量作为适应度函数,交叉与变异仅针对点列的相对关系完成,提出用局部适应度函数自适应调整交叉概率与变异概率.仿真结果表明,该方法可以有效完成地磁匹配导航中任意形状路径的匹配.     

Solar cycle and latitude dependence of high-beta suprathermal plasma conditions in interplanetary space between 1.3 and 5.4 AU

The analysis of energetic particles and magnetic field measurements from the Ulysses spacecraft has shown that in a series of events, the energy density contained in the suprathermal tail particle distribution is comparable to or larger than that of the magnetic field, creating conditions of high-beta plasma. In this work we analyze periods of high-beta suprathermal plasma occurrences (β_ep > 1) in interplanetary space, using the ratio (β_ep) of the energetic particle (20 keV to ∼5 MeV) and magnetic field energy densities from measurements covering the entire Ulysses mission lifetime (1990–2009) in order to reveal new or to reconfirm some recently defined interesting characteristics. The main key-results of the work are summarized as follows: (i) we verify that high-beta events are detected within well identified regions corresponding mainly to the vicinity of shock surfaces and magnetic structures, and associated with energetic particle intensity enhancements due to (a) reacceleration at shock-fronts and (b) unusually large magnetic field depressions. (ii) We define three considerable features for the high-beta events, concentrated on the next points: (a) there is an appreciable solar-activity influence on the high-beta events, during the maximum and middle solar-cycle phase, (b) the annual peak magnitude and the number of occurrences of high events are well correlated with the sunspot number, (c) the high-beta suprathermal plasma events present a spatial distribution in heliographic latitudes (HL) up to ∼±80°, and a specific important concentration on the low (−25° ? HL < −6°, 6° < HL ? 25°) and median (−45° ? HL < −25°, 25° < HL ? 45°) latitudes. We also reconfirm by a statistical analysis the results of Marhavilas and Sarris (2011), that the high-beta suprathermal plasma (β_ep > 1) events are characterized by a very large parameter β_ep (up to 1732.5), a great total duration (406 days) and a large percentage of the Ulysses-mission lifetime (which is equal to 6.34% of the total duration with usable measurements, and 11.3% of the duration in presence of suprathermal particles events).     

A heuristic derivation of an improved analytical theory for perpendicular diffusion of charged particles

A heuristic derivation of an improved nonlinear guiding center theory for perpendicular diffusion of charged particles is presented. This new derivation complements previous work which is based on an indirect solution of the Fokker–Planck equation. The new derivation confirms the improved theory for diffusion of charged particles and makes the validity of the theory plausible.     

Features of mass supply and flows related with reconnection in the solar corona

Symmetrical broadening in the emission spectral lines is the ultimate observational effect of magnetic reconnection in the solar corona. Reconnection can create plasmas of very different temperatures and, hence, very different electrical conductivities in the corona. The electrodynamical effect of such a mass supply is considered. Electromagnetic expulsion force, different from Parker's well-known magnetic buoyancy force, can effectively balance gravity in prominences and generate fast vortex flows in the vicinity of fine threads inside prominences. The possibility of observing this effect from SOHO is discussed.     

Evolution of binaries with chemically peculiar primaries

The chemically peculiar (CP) stars are classified into subgroups based on the type of peculiarities. A significant fraction of these are known to be binaries. The faster evolution of the massive component leads to a white dwarf or a neutron star. Further evolution of the binary is analysed taking into consideration, the orbital parameters, effect of magnetic field, spectroscopic peculiarities and finally the statistics of CP binaries and Low Mass X-ray Binaries (LMXB).

The possible consequences of the evolution to lead to the formation of Magnetic Cataclysmic Variables (MCV) and LMXB are discussed.