Theoretical Advances in Prominence Seismology

Prominence seismology is a rapidly developing topic which seeks to infer the internal structure and properties of solar prominences from the study of its oscillations. An extensive observational background about oscillations in quiescent solar prominences has been gathered during the last 70 years. These observations point out the existence of two different types of oscillations: Flare-induced oscillations (winking filaments) which affect the whole prominence and are of large amplitude and small amplitude oscillations which seem to be of local nature. From the theoretical point of view, few models have been set up to explain the phenomenon of winking filaments while, on the contrary, for small amplitude oscillations a large number of models trying to explain the observed features have been proposed.     

用凝固模拟方法预测铝合金铸件缩松的形成

用有限元法和六节点等参数单元对铝合金金属型铸造过程进行了温度场的数值模拟，对铸件不同典型部位进行了金相分析，结果表明，参数Ｇ／可有效地预测铝合金缩松形成倾向的大小，计算值与实测值基本一致。     

Properties of Interplanetary Coronal Mass Ejections

Interplanetary coronal mass ejections (ICMEs) originating from closed field regions on the Sun are the most energetic phenomenon in the heliosphere. They cause intense geomagnetic storms and drive fast mode shocks that accelerate charged particles. ICMEs are the interplanetary manifestations of CMEs typically remote-sensed by coronagraphs. This paper summarizes the observational properties of ICMEs with reference to the ordinary solar wind and the progenitor CMEs.     

Microphysics of Magnetic Reconnection

Magnetic reconnection is a universal phenomenon where energy is efficiently converted from the magnetic field to charged particles as a result of global magnetic topology changes during which earlier separated plasma regions become magnetically connected. While the reconnection affects large volumes in space most of the topology changes and of the energization occur within small localized regions. Regions of special importance are the X-region and the separatrix region. The understanding of the microphysics of these regions is crucial for the overall understanding of the reconnection. The Earth magnetosphere is the best environment where the details of these regions can be studied in situ. We summarize their main properties and discuss recent spacecraft observations.     

Neutron stars: Classification and evolution

The general aproach is considered which describs the evolution of neutron stars in terms of their interaction with surrounding matter. All possible states of neutron stars are classified from this point of view. Classification and evolution of binaries contaning neutron stars are also considered.     

Physical processes in the strong magnetic fields of accreting neutron stars

The key radiative processes are discussed, numerical methods of magnetized radiative transfer are presented, and these are considered in their application to X-ray pulsar models.     

Direct integration methods in dynamic problems of structural mechanics

A method of direct integration with respect to time is proposed to solve dynamic problems of structural mechanics and comparison with the well-known methods is presented.     

多尺度子域基函数矩量法解的稳定性与迭代法

通过对几个具体实例的计算，证实了在电磁场边值问题的矩量法求解过程中，选用不同的基函数其解的数值稳定性会有很大的差别。从而有可能选择一种数值稳定性比较好的基函数来进行矩量法求解。另一方面，提出了选用多尺度子域基函数，并通过多次迭代来提高矩量法解的精度的算法。实例计算表明，该算法不仅可以有效地降低系数矩阵的条件数，而且还降低了对计算机内存容量的要求，是一种有效的、稳定的算法     

大功率无电极高密度等离子体电磁推进概述

无电极高密度等离子体电磁推进技术已成为未来深空探测、载人航天和货运、太阳能电站以及航天器在轨服务与维护等空间任务中极具竞争力的核心推进技术之一。在梳理不同无电极等离子体电磁加速机制基础上,开展大功率无电极高密度等离子体电磁推进技术性能对比,给出新概念无电极场反构型电磁推进技术向未来超大功率拓展的优势和发展潜力,同步分析了该技术亟需解决的关键基础问题,旨在为中国新概念场反构型电磁推进技术的研发提供理论基础。     

基于空间两点的视觉自主着陆导引算法设计

为提高无人机着陆效率,从着陆速度向量场和导引律设计两方面研究改进。首先,基于椭圆设计速度向量场,实现飞行路程更短、机动性能要求更低的着陆轨迹。然后,基于像素坐标系与机体坐标系的关系,设计无人机的航迹方位角指令;以椭圆切线方向为参考,结合合作矢量特征,设计航迹倾斜角指令;利用图像信息,设计速度大小指令。最后,理论比较了传统轨迹与提出轨迹对方向机动性性能的要求,给出了轨迹参数与无人机方向机动性性能的关系。利用Simulink搭建系统仿真平台,计算满足要求的合作矢量特征。结果表明,无人机以曲线轨迹准确软着陆到目标,满足实际运用的需要。