Modelling and observations of photospheric magnetic helicity

Mounting observational evidence of the emergence of twisted magnetic flux tubes through the photosphere have now been published. Such flux tubes, formed by the solar dynamo and transported through the convection zone, eventually reach the solar atmosphere. Their accumulation in the solar corona leads to flares and coronal mass ejections. Since reconnections occur during the evolution of the flux tubes, the concepts of twist and magnetic stress become inappropriate. Magnetic helicity, as a well preserved quantity, in particular in plasma with high magnetic Reynolds number, is a more suitable physical quantity to use, even if reconnection is involved.     

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.     

可伸缩式转移居住舱结构方案的探讨

描述了一种新型的可伸缩式居住舱－可充气式转移居住舱（TransHab)。该项目可用于星际间的转移居住舱，也可装配到空间站上。发射时，所有要用到的仪器设备提前装入舱内，整个舱体呈收缩状态装入航天飞机的货舱内，待入轨后，舱体像气球一样充气展开。展开后舱体的容积大，而质量却轻得多。本文着重讨论了这种可充气转移居住舱的基本结构形式，并与其他几种美国先前研制的可伸缩结构进行了比较。提出了该种类型结构形式的技术难点，发展前景，以及我国进行该种结构研究的必要性。     

神经网络在下颌运动轨迹图测量中的应用

介绍了采用小型磁石测量下颌运动轨迹图Electrognathography(EGN)的方法。给出利用磁偶极子模型代替小磁石模型的理论及实际依据。利用神经网络解决由磁石产生的磁感应强度推定其空间参数的反演问题 ,并且采用了分割网络及修正网络的方法来提高磁石运动测量的推定准确度。     

柔性多层冲击空间碎片防护结构设计与试验

充气展开密封结构是未来空间站以及大型空间居住舱的理想构建形式,其外蒙皮由气密层、增强层、微流星体和空间碎片防护层、辐射保护层以及热控层组成。为了既满足对空间碎片的防护,又满足折叠、收纳以及展开的要求,空间碎片防护层需要采用多层冲击防护结构设计。基于多层冲击防护结构,采用国产的玄武岩纤维材料和芳纶织物的特性参数,根据弹道极限方程设定了柔性空间碎片防护层的设计参数,并通过高速撞击试验对根据设计参数生产的试验件进行了试验验证,试验结果与柔性多层冲击防护结构的弹道极限方程吻合较好。     

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。     

小型磁偏转质谱计性能实验研究

自主研发了小型磁偏转质谱计，并对其质量范围、分辨本领、灵敏度和最小可检分压力四个主要性能指标进行了实验测试和比对。结果表明，该质谱计的质量范围为（1~143）amu，相对N₂的分辨本领为1400，灵敏度为4.2×10^-5 A/Pa，最小可检分压力为9.5×10^-7 Pa。该测试和比对结果为磁偏转质谱计进一步的优化设计和性能提高奠定了重要基础。     

改善横向波纹隔热屏综合冷却效率的发散冷却结构优化

为改善横向波纹隔热屏综合冷却效果，采用三维数值模拟和基于支持向量机的代理优化模型，在给定的单位面积冷却空气流量下对发散冷却结构参数进行了优化研究。设计变量选取为气膜孔直径、气膜孔排布的展向间距和流向间距，以面积平均综合冷却效率作为目标函数，通过遗传算法搜索获得了设计变量区间内的优化设计点。在隔热屏单位表面积冷却空气流量G_f = 2.647 kg/（m²?s）的工况下，优化后的d、P和S分别为0.8、4和5 mm。研究结果表明，优化的隔热屏冷却结构应具有较小的气膜孔直径d和展向间距P，以及适中的流向间距S。相对于参考结构，优化后的发散冷却结构能够改善沿流向的气膜覆盖，缩减发散冷却起始段局部高温段，起到增强隔热屏发散冷却综合冷却效率的作用。     

Plasma transport process in the equatorial/low-latitude ionosphere

The behaviour of the equatorial/low-latitude ionosphere and the transport processes during magnetic disturbed and quiet periods of a high solar activity year, 2014, in the American sector are investigated. Parameters used include vertical drift (Vz), transport term (W), NmF2, hmF2 and scale-height (H). The F2 plasma variations followed the diurnal local solar pattern, being higher at daytime. The sunset maximum and sunrise minimum peaks of hmF2 were directly opposite to the scale height (H) pattern. The plasma distribution was basically controlled by combined actions of the electrodynamic convection/thermospheric composition, which is geomagnetic activity dependent. The annual, semi-annual and winter-anomalies of the F2 parameters were higher at the dip equator in comparison with the low-latitude. The Vz pre-reversal peak magnitude coincided with hmF2 peak and the effects are more pronounced during geomagnetic disturbed conditions. The transport term pattern was similar to that of the scale height and it is suggested as a proxy parameter for quantifying low-latitude plasma irregularities and distribution of thermospheric composition.