Viewing radiation signatures of solar energetic particles in interplanetary space

A current serious limitation on the studies of solar energetic particle (SEP) events is that their properties in the inner heliosphere are studied only through in situ spacecraft observations. Our understanding of spatial distributions and temporal variations of SEP events has come through statistical studies of many such events over several solar cycles. In contrast, flare SEPs in the solar corona can be imaged through their radiative and collisional interactions with solar fields and particles. We suggest that the heliospheric SEPs may also interact with heliospheric particles and fields to produce signatures which can be remotely observed and imaged. A challenge with any such candidate signature is to separate it from that of flare SEPs. The optimum case for imaging high-energy (E > 100 MeV) heliospheric protons may be the emission of π⁰-decay γ-rays following proton collisions with solar wind (SW) ions. In the case of E > 1 MeV electrons, gyrosynchrotron radio emission may be the most readily detectible remote signal. In both cases we may already have observed one or two such events. Another radiative signature from nonthermal particles may be resonant transition radiation, which has likely already been observed from solar flare electrons. We discuss energetic neutrons as another possible remote signature, but we rule out γ-ray line and 0.511 MeV positron annihilation emission as observable signatures of heliospheric energetic ions. We are already acquiring global signatures of large inner-heliospheric SW density features and of heliosheath interactions between the SW and interstellar neutral ions. By finding an appropriate observable signature of remote heliospheric SEPs, we could supplement the in situ observations with global maps of energetic SEP events to provide a comprehensive view of SEP events.     

新型磁性液体材料的研究与探讨

磁性液体，是由固体的磁性粒子分散到载体（液体）中形成的一种胶体溶液，此种深夜既有液体的流动性，又具有磁性，是一种新型的磁性材料，本文对磁性液体的制造方法，及其存在的条件，进行了研究与探讨，并简单介绍了磁性液体的性质及其应用前景。     

太阳宁静区磁漏斗结构的扩展特征

通过对观测的光球纵向磁场进行势场外推, 重构了一个太阳宁静区光球以上的磁场结构. 结果显示, 在20 Mm 以下, 开放磁力线呈现多个明显的小磁漏斗结构, 这些小磁漏斗结构随高度扩展, 并且在20 Mm 左右融合成大的漏斗结构. 通过系统地研究磁漏斗结构横截面积随高度的变化趋势, 发现太阳宁静区磁漏斗结构的截面积随高度近似线性扩展, 磁漏斗结构在较低高度上(<20Mm) 扩展的速度比在较高高度上 (>20Mm) 扩展的速度要快. 这一结果对太阳风起源和磁环中物质流动的二维数值模拟具有重要的意义. 同时还发现, 闭合磁力线的数目随高度以指数函数的形式减少.     

等离子体彗尾流线断裂现象的讨论

等离子体Ⅰ型彗尾流线的断裂,已多次被人们见到.本文用MHD的理论,讨论和分析了这种现象,认为这是一种空间等离子体扰动所产生的结果.本文作了定性的分析,及定量的计算,比较满意地解释了这种彗尾中的观测现象.     

Geoeffectivity of Coronal Mass Ejections

Coronal mass ejections and post-shock streams driven by them are the most efficient drivers of strong magnetospheric activity, magnetic storms. For this reason there is considerable interest in trying to make reliable forecasts for the effects of CMEs as much in advance as possible. To succeed this requires understanding of all aspects related to CMEs, starting from their emergence on the Sun to their propagation to the vicinity of the Earth and to effects within the magnetosphere. In this article we discuss some recent results on the geoeffectivity of different types of CME/shock structures. A particularly intriguing observation is that smoothly rotating magnetic fields within CMEs are most efficient in driving storm activity seen in the inner magnetosphere due to enhanced ring current, whereas the sheath regions between the shock and the ejecta tend to favour high-latitude activity.     

基于双磁钢转子的大力矩飞轮用电机设计

针对卫星快速敏捷和大角度机动的需求,设计了一种基于双磁钢转子的大力矩飞轮用永磁电机。介绍了大力矩飞轮用电机的工作原理和结构构成,给出了主要尺寸的设计准则,并在Maxwell 环境下对双磁钢转子的永磁直流电动机进行了有限元分析。     

弧齿锥齿轮齿面拓扑修形及加工参数计算

为了能够实现对齿面啮合性能的灵活控制,针对弧齿锥齿轮小轮提出一种齿面拓扑修形方法,即借助二阶曲面对齿面偏差拓扑的近似表达,将齿面拓扑修形分解为5个方向:螺旋角修正、压力角修正、齿长曲率修正、齿廓曲率修正及齿面挠率修正,通过改变5个方向的修形系数对小轮齿面拓扑结构进行自由控制。在此基础上,建立齿面偏差与机床加工参数之间的修正数学模型,通过构建敏感性矩阵并采用最小二乘法求解,反求出获得修形齿面的小轮加工参数,以便指导加工。以一对弧齿锥齿轮副为例进行修形啮合分析,仿真结果表明:选取齿长曲率修形系数为0.0001,齿廓曲率修形系数为0.0005,齿面挠率修形系数为0.0003,对齿面进行拓扑修形后传动误差幅值为-25.60″,接触迹线倾斜角度变为54.7°,相比原始结果啮合性能得到改善。滚检接触区与理论仿真结果一致,验证了修形方法的有效性。      

强场脉冲充磁退磁装置

介绍了充电电容器通过磁路瞬时放电产生强磁场的原理 ,选择回路参数可实现高矫顽力类永磁材料的充磁或者退磁 ,介绍了所研制的脉冲充磁退磁装置的性能。     

星间洛仑兹力编队飞行的平衡点及零速度曲面

提出了一种新的利用星间洛仑兹力控制卫星相对运动的方法:使主星产生自旋磁场,副星带电,通过控制副星所受的星间洛仑兹力进行编队。假设主星产生的人造磁场表现为偶极子并且运动在一条开普勒圆形轨道上,副星恒定带电并在主星附近运动,同时假设星间洛仑兹力只影响副星的运动而不影响主星的运动。推导了副星在主星HCW(当地垂直当地地平坐标系)坐标系下的相对运动动力学方程。针对偶极子与HCW坐标轴X轴重合的情况下,推导了动力系统下的平衡点(并采用稳定性分析方法分析其线性化意义下的稳定性)、积分常数和零速度曲面,证明了有界相对运动的存在。最后用数值仿真验证了上述结论。     

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。