22太阳周极大期Imp≥M1.0X射线耀斑的分布特征

本文对第22太阳周极大时期Imp≥M1.0X射线耀斑的空间分布进行了统计分析.结果表明,该事件存在南北半球分布的不对称性,且不对称性在极大年或其后一年改变符号.文中还对不对称性与太阳活动的相关关系也进行了探讨.      

质心干扰对抗现代反舰导弹的一种改进方法

分析了质心干扰的作用过程以及质心干扰在对抗现代反舰导弹中存在的不足,提出了质心干扰的一种改进方法:即利用箔条幕对电磁波的衰减特性,遮挡目标舰,降低目标舰的雷达反射截面积,而利用散射型箔条云作为质心诱饵。     

Fabrication and Investigation on Double-Hollow Shell CoFe Oxide@TiO2 Nanocube with Superior Electromagnetic Properties

Electromagnetic wave absorbing materials are urgently required in the fields of medicine, communication, and military. However, the thickness, weight, narrow effective bandwidth, and weak absorbing ability of the materials restrict their further application. In this work, a double-layer hollow nanocube with a dielectric titanium dioxide (TiO2) shell and a magnetic CoFe oxide inner shell is prepared. Prussian blue (PB) is prepared by the hydrothermal method, and used as the template to prepare PB@CoFe PB analogue (PBA). After selective etching and further calcination, hollow CoFe oxide particles are obtained. The obtained particles are then coated with SiO2 and TiO2, respectively, and the intermediate layer is dislodged to obtain the final CoFe oxide@TiO2 with the hollow double shell structure. The obtained double-layer hollow structure can effectively capture the incident electromagnetic waves, and increase the propagation path. Moreover, the obvious enhancement of interface polarization and the improvement of impedance matching enhance the wave absorbing ability of the material. The analysis results show that, the structure is stable and the dispersion is good. The maximum reflection loss (RL) at 10 GHz is as high as -46.1 dB with the sample thickness of 1.6 mm. The light-weight and high-efficiency CoFe oxide@TiO2 absorber is promised to be used in commercial and military aerospace fields.     

Transient Effects and Disturbed Conditions

In the present phase of the solar cycle no big transients leading to strong modulation had been observed after 1991. Apart from a few minor disturbances cosmic rays were still recovering to a new intensity maximum. It was suggested, therefore, that existing literature from previous cycles should be critically reviewed. The scene was set by the introductory papers on— phenomenology of cosmic ray modulation in successive solar cycles throughout the heliosphere— the present state of models for long term modulation and their shortcomings— the relation between cosmic ray variations and the magnitude of the interplanetary magnetic field (the CR-B-relation)— charge dependent effects.In the discussions, the study of propagating diffusive disturbances and the CR-B-relation played a central role. The difference was stressed between isolated transient disturbances in the inner solar system (Forbush decreases), and the long lasting, step-like decreases caused by merged interaction regions in the outer heliosphere. The recovery rates following the step-like decreases vary with the phase in the 22-year solar cycle. In some cases this requires a modification of existing drift models. In the outer heliosphere, the CR-B-relation leads to the result 1/ between the diffusion coefficient and the field magnitude . This simple result is a challenge for theoreticians to derive the perpendicular diffusion coefficient fromfirst principles. The three articles in this report essentially follow the list of open points and arguments just presented.The article "Observations and Simple Models" is organised around the model of a propagating diffusive barrier, its application to Forbush effects in the inner heliosphere and to decreases caused by merged interaction regions in the outer heliosphere. Acomparison of observed Forbush decreases with model predictions requires a careful separation of the two steps related to the turbulent region behind the shock front and the closed magnetic field regions of the ejecta (the interplanetary counterparts of coronal mass ejections). It is shown that models for propagating disturbances can be used to derive values of the diffusion coefficients phenomenologically, not only during the disturbance, but also in the ambient medium.The "Modeling of Merged Interaction Regions" summarizes the dynamic and time-dependent process of cosmic ray modulation in the heliosphere. Numerical models with only a time-dependent neutral sheet prove to be successful when moderate to low solar activity occurs but fail to describe large and discrete steps in modulated cosmic rays when solar activity is high. To explain this feature of heliospheric modulation, the concept of global merged interaction regions is required. The com-bination of gradient, curvature and neutral sheet drifts with these global merged interaction regions has so far been the most successful approach in explaining the 11-year and 22-year cycles in the long-term modulation of cosmic rays.The "Remarks on the Diffusion Tensor in the Heliosphere" describe available theories of perpen-dicular diffusion and drift, and discuss their relevance to cosmic rays in the heliosphere. In addition, the information about diffusion coefficients and spatial gradients obtained from the analysis of steady state anisotropies at neutron monitor energies is summarized. These topics are intimately related to the other two articles. They are also part of the general discussion about the "Diffusion Tensor throughout the Heliosphere" which played an important role in all working groups.     

The Solar Wind - Inner Heliosphere

The solar wind in the inner heliosphere, inside ~ 5 AU, has been almost fully characterized by the addition of the high heliographic latitude Ulysses mission to the many low latitude inner heliosphere missions that preceded it. The two major omissions are the high latitude solar wind at solar maximum, which will be measured during the second Ulysses polar passages, and the solar wind near the Sun, which could be analyzed by a Solar Probe mission. Here, existing knowledge of the global solar wind in the inner heliosphere is summarized in the context of the new results from Ulysses.     

Fractionation of SI, NE, and MG Isotopes in the Solar Wind as Measured by Soho/Celias/MTOF

Using the high-resolution mass spectrometer CELIAS/MTOF on board SOHO we have measured the solar wind isotope abundance ratios of Si, Ne, and Mg and their variations in different solar wind regimes with bulk velocities ranging from 330 km/s to 650 km/s. Data indicate a small systematic depletion of the heavier isotopes in the slow solar wind on the order of (1.4±1.3)% per amu (2σ-error) compared to their abundances in the fast solar wind from coronal holes. These variations in the solar wind isotopic composition represent a pure mass-dependent effect because the different isotopes of an element pass the inner corona with the same charge state distribution. The influence of particle mass on the acceleration of minor solar wind ions is discussed in the context of theoretical models and recent optical observations with other SOHO instruments. This revised version was published online in June 2006 with corrections to the Cover Date.     

硝酸铵喷雾干燥表面改性

为降低硝酸铵、（AN）的吸湿性，采用喷雾干燥技术，用聚合物和偶联剂对相稳定硝酸铵（PSAN）进行改性。通过吸湿性、接触角、包覆层质量百分数、XPS和SEM对改性后的PSAN进行了表征，研究结果表明，用偶联剂和聚合物对PSAN进行复合表面改性可有效抑制PSAN的吸湿，改性后平均相对吸湿率为46%，比用液相沉积法平均下降了约3%，包履层质量下降了76%，说明喷雾干燥技术的改性效果明显优于液相沉积技术。     

镉镍电池正极浸渍液中钴含量的分析

简述了运用AIR－C2H2原子吸收光谱法进行镉镍电池正极浸渍液中钴含量的测试，分析了钴最佳测定条件以及呈良好线性范围的浓度，同时对样品消化处理条件，干扰因素进行了综合考虑，实验表明，该方法具有很好的灵敏度，重现性，干扰小，方法简单，操作容易掌握等特点。对样品然含量的测定，相对标准偏差均小于1．0％（n=6)，标准加入回收率均在97．0％－102．0%(n=5)范围内，达到了实验室分析质量控制的要求，完全适用于镉镍电池正极浸渍液中钴含量的控制分析和样品系统分析。     

氰酸酯树脂在宇航复合材料中的应用

氰酸酯树脂是一种新型高性能宇航复合材料树脂基体。本文介绍了氰酸酯树脂的种类,聚合机理,性能特点及应用概况。重点综述了氰酸酯树脂基复合材料在宇航电子设备用的高性能印刷电路板,宇航结构部件,隐身材料,雷达罩和人造卫星等方面的应用情况和发展方向。     

Coronal plumes and fine scale structure in high speed solar wind streams

We present a solar wind model which takes into account the possible origin of fast solar wind streams in coronal plumes. We treat coronal holes as being made up of essentially 2 plasma species, denser, warmer coronal plumes embedded in a surrounding less dense and cooler medium. Pressure balance at the coronal base implies a smaller magnetic field within coronal plumes than without. Considering the total coronal hole areal expansion as given, we calculate the relative expansion of plumes and the ambient medium subject to transverse pressure balance as the wind accelerates. The magnetic flux is assumed to be conserved independently both within plumes and the surrounding coronal hole. Magnetic field curvature terms are neglected so the model is essentially one dimensional along the coronal plumes, which are treated as thin flux-tubes. We compare the results from this model with white-light photographs of the solar corona and in-situ measurements of the spaghetti-like fine-structure of high-speed winds.