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.     

碳/环氧复合材料两次表面镜基板研制

文章介绍了碳/环氧复合材料两次表面镜基板的结构与铺层、选材与成型工艺,性能测试等内容。     

纤维增强复合材料电子束固化工艺

纤维增强复合材料电子束固化工艺采用电子加速器给电子以足够的能量使树脂体系发生交联反应而固化。该工艺不需要热压罐,可在室温下固化。从而降低模具费用,节省能源,减小制品中的热应力,制品综合性能好,是纤维增强复合材料低成本生产的一种新颖方法。电子束固化的基本条件是要有可被电子束固化的树脂体系和电子加速器,该方法已被用来生产大型空间运载器的结构部件。     

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。     

Thermal cyclotron radiation from a hot coronal loop with helical magnetic field

The spectral and polarization properties of thermal cyclotron radio emission from a hot coronal loop with a current along the axis are computed. The magnetic field is supposed to have a component along the loop axis as well as a poloidal part due to the current, both components being of comparable magnitude. In this specific configuration a helical magnetic field is present with a remarkable minimum of its absolute value along the loop axis and a maximum at its periphery. The presence of one or two maxima of magnetic field value along the line of sight results in increasing optical thickness of the gyroresonance layers at appropriate frequencies in the microwave band and, therefore, in enhanced radio emission at those harmonics which are optically thin (for example,s=4). These cannot be observed in models with the commonly employed magnetic field configuration (longitudinal along the loop axis).We show that the frequency spectrum of thermal cyclotron radiation from a hot coronal loop with a helical magnetic field differs from that of the standards-component source (with smooth frequency characteristics and polarization corresponding toe-mode) in that plenty of fine structures (line-like features and cut-offs) are present and theo-mode is prevalent in some frequency intervals. The enhanced radio emission at high harmonics and the complicated form of frequency spectrum in the model considered imply that some microwave sources, which are poorly explained in traditional models of solar active regions, may be associated with helical magnetic fields in hot coronal loops. Computations allow one to indicate spectral and polarizational peculiarities of local sources testifying to the presence of a helical magnetic field.     

窄分布纳米级HMX的制备及粒度分析

通过撞击法成功地制备了窄分布的纳米级HMX。实验结果表明，分散剂1和分散剂2能改善HMX的粒度分布。在分散剂1存在的条件下，用撞击法可制备出粒度分布较窄的纳米HMX颗粒，其d50分别为70．1nm和68．9nm，分布范围分别为0．9nm和1．4nm。     

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.     

对中国航空材料体系构建中若干问题的看法与建议

阐述了构建中国航空材料体系所要实现的四项目标、所要解决的四个问题以及需要处理好五个关系,并对构建的具体步骤与方法提出了建议.     

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.