Modelling of the electromagnetic field in the interplanetary space and in the Earth's magnetosphere

A magnetohydrodynamic model of the solar wind flow is constructed using a kinematic approach. It is shown that a phenomenological conductivity of the solar wind plasma plays a key role in the forming of the interplanetary magnetic field (IMF) component normal to the ecliptic plane. This component is mostly important for the magnetospheric dynamics which is controlled by the solar wind electric field. A simple analytical solution for the problem of the solar wind flow past the magnetosphere is presented. In this approach the magnetopause and the Earth's bow shock are approximated by the paraboloids of revolution. Superposition of the effects of the bulk solar wind plasma motion and the magnetic field diffusion results in an incomplete screening of the IMF by the magnetopause. It is shown that the normal to the magnetopause component of the solar wind magnetic field and the tangential component of the electric field penetrated into the magnetosphere are determined by the quarter square of the magnetic Reynolds number. In final, a dynamic model of the magnetospheric magnetic field is constructed. This model can describe the magnetosphere in the course of the severe magnetic storm. The conditions under which the magnetospheric magnetic flux structure is unstable and can drive the magnetospheric substorm are discussed. The model calculations are compared with the observational data for September 24–26, 1998 magnetic storm (Dst _min=−205 nT) and substorm occurred at 02:30 UT on January 10, 1997. This revised version was published online in August 2006 with corrections to the Cover Date.     

高温相变单元管蓄热过程数值模拟

对以高温共晶盐 Li F-Ca F2 为相变材料 (PCM)和以干空气为工质的相变蓄热系统 ,采用焓方法建立了以控制体单元为对象的单管相变蓄热模型。在模拟空间站太阳能吸热 /储热器轨道运行参数下进行了数值计算。计算结果与地面模拟试验数据进行了比较 ,吻合良好。     

Composition Variations in the Solar Corona and Solar Wind

Order of magnitude variations in relative elemental abundances are observed in the solar corona and solar wind. The instruments aboard SOHO make it possible to explore these variations in detail to determine whether they arise near the solar surface or higher in the corona. A substantial enhancement of low First Ionization Potential (FIP) elements relative to high FIP elements is often seen in both the corona and the solar wind, and that must arise in the chromosphere. Several theoretical models have been put forward to account for the FIP effect, but as yet even the basic physical mechanism responsible remains an open question. Evidence for gravitational settling is also found at larger heights in quiescent streamers. The question is why the heavier elements don't settle out completely. This revised version was published online in June 2006 with corrections to the Cover Date.     

UVCS/SOHO Observations of Spectral Line Profiles in Polar Coronal Holes

Ultraviolet emission line profiles have been measured on 15-29 September 1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar coronal hole, at heliographic heights ? (in solar radii) between 1.34 and 2.0. Observations of H I 1216 Å and the O VI doublet from January 1997 for ? = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is observed to have a narrow component at ? = 1.34 which accounts for only a small fraction of the observed spectral radiance, and a broad component that exists at all observed heights. The widths of O VI broad components are only slightly larger than those for H I at ? = 1.34, but are significantly larger at ? = 1.5 and much larger for ? > 1.75. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least ? = 2.0, but never reach the values of O VI.     

太阳能火箭发动机聚光器设计方法

对工程上常用聚光器进行了性能比较,得出了适合于太阳能火箭发动机(STP)的聚光器及其具有的性能优点,研究了此种聚光器的的设计方法,并推出了相关公式和其中的关键技术,这对STP聚光器的工程设计具有重要的指导价值。      

基于共轭循环平稳特性的二维波达方向估计方法

 提出了一种具有阵列孔径扩展能力的共轭循环平稳二维波达方向（DOA）估计方法。该方法通过引入伪采样,充分利用了阵元输出之间共轭循环互相关函数的时间维信息,扩展了阵列有效孔径,提高了算法DOA估计精度,具有较好的低信噪比适应能力。该方法避免了最优时延选择问题,无需谱峰搜索,且其二维角度参数能够自动配对,具有较低的计算量。计算机仿真结果验证了该方法的有效性。     

Solar and Solar-Wind Composition Results from the Genesis Mission

The Genesis mission returned samples of solar wind to Earth in September 2004 for ground-based analyses of solar-wind composition, particularly for isotope ratios. Substrates, consisting mostly of high-purity semiconductor materials, were exposed to the solar wind at L1 from December 2001 to April 2004. In addition to a bulk sample of the solar wind, separate samples of coronal hole (CH), interstream (IS), and coronal mass ejection material were obtained. Although many substrates were broken upon landing due to the failure to deploy the parachute, a number of results have been obtained, and most of the primary science objectives will likely be met. These objectives include He, Ne, Ar, Kr, and Xe isotope ratios in the bulk solar wind and in different solar-wind regimes, and ¹⁵N/¹⁴N and ¹⁸O/¹⁷O/¹⁶O to high precision. The greatest successes to date have been with the noble gases. Light noble gases from bulk solar wind and separate solar-wind regime samples have now been analyzed. Helium results show clear evidence of isotopic fractionation between CH and IS samples, consistent with simplistic Coulomb drag theory predictions of fractionation between the photosphere and different solar-wind regimes, though fractionation by wave heating is also a possible explanation. Neon results from closed system stepped etching of bulk metallic glass have revealed the nature of isotopic fractionation as a function of depth, which in lunar samples have for years deceptively suggested the presence of an additional, energetic component in solar wind trapped in lunar grains and meteorites. Isotope ratios of the heavy noble gases, nitrogen, and oxygen are in the process of being measured.     

太阳能飞机翼肋结构拓扑优化设计

太阳能飞机翼肋结构轻薄且数量众多,其结构形式的合理性对于结构减重、机翼刚度设计等具有重要意义。基于现有太阳能飞机翼肋的结构形式,提出一种翼肋拓扑优化设计方法:首先,应用双向渐进结构优化法(BESO),以单元应力为判断指标,对太阳能飞机典型翼肋进行结构拓扑优化;其次,基于拓扑优化结果对翼肋进行结构细节设计;最后,通过有限元计算,验证翼肋的结构强度、刚度和静稳定性。通过本文方法,能够得到太阳能飞机翼肋更为合理的结构布局。     

应召反潜时无人机监听航路的规划

浮标阵是航空反潜模式下应召搜潜时常用的一种反潜手段。在假设浮标阵已被布设完毕并且由无人机对其进行实时监听的前提下,文章重点研究了无人机监听航线的规划问题。首先,研究了浮标阵的布设及其特点,分析了无人机航路的代价问题;接着,根据浮标阵的特点规划出了无人机监听方形浮标阵的监听航路飞行方案,并对所规划航路的技术指标进行了分析和研究;最后,对无人机的监听航路进行了计算,计算结果表明文中所规划的方案是可行的,这为无人机监听浮标阵的实际应用提供了参考。     

一种新型超宽带紧耦合天线阵列设计

针对紧耦合天线阵列（Tightly Coupled Array,TCA）安装于飞机、导弹、舰船等平台时接地板严重影响其阻抗带宽的问题,将栅格形阻性频率选择表面与交指型偶极子天线单元相结合,设计了一种新型多层结构的超宽带TCA。采用CST对加载与未加载栅格形阻性频率选择表面时TCA的性能进行了比较分析。结果表明：未加载时,受接地板影响其最佳阻抗带宽（VSWR〈2）为4．5：1（2．1～9．5GHz）;加载后,TCA可克服接地板的影响,其阻抗带宽可达10．4：1（1．8～18．8GHz）。