某民用飞机机身典型壁板压损分析

通过RADIOSS显示有限元计算,对典型壁板结构的承载能力进行了计算分析,并与试验结果进行对比,验证了RADIOSS显式有限元计算分析的准确性。在此基础上,针对某民用飞机的机身壁板5种不同的典型壁板结构,分别在长度为200 mm和530 mm的情况下,采用有限元分析方法计算了长桁及壁板结构的压损和失稳情况,最终得出5种构型下的压损及失稳结果,为机身结构共性结构选型提供了数据支持。     

FGM板三维层合模型及热-噪声载荷下的动态响应研究

 为了有效地分析热-噪声联合载荷作用下的飞行器功能梯度壁板结构的非线性动态响应,提出了运用复合材料多层壳单元建立功能梯度材料(FGM)板的层合有限元建模新方法,研究了FGM板在热曲屈前、后状态下复杂的非线性时域动态响应特性,并探讨了梯度指数、热曲屈系数及声压级(SPL)等参数对FGM板非线性动态跳变响应的影响规律。FGM板三维层合建模新方法避免了采用常规有限元法(FEM)建模时需要在厚度方向划分大量单元的缺点;求解FGM板非线性动态响应时采用的隐式积分方案避免了模态叠加法对参与模态选择的经验性要求及模态截断造成的信息丢失等缺陷。仿真结果表明:FGM板层合有限元建模新方法合理可行、过程简便、计算精度高;研究发现:陶瓷-金属FGM板在热屈曲后的抗声振性能并不像热屈曲前那样介于金属板和陶瓷板之间,而是表现最差;热屈曲系数及声压级的组合形式是导致FGM板发生非线性跳变响应的主要影响因素。     

大尺寸C/ E 面板铝蜂窝夹层结构筒形件成型工艺

对某大尺寸MT300碳纤维/648环氧树脂面板蜂窝夹层结构筒形件成型工艺进行研究,介绍了内外面板成型工艺、“F”形前后金属端框与铝蜂窝夹芯插接工艺以及“F”形前后金属端框、内外面板与蜂窝夹芯的组装整体固化技术.通过模具设计优化大尺寸夹层结构筒形件尺寸满足设计要求,并解决了内外面板-蜂窝夹芯-前后金属框组装整体固化技术成型难点.     

Type II Solar Radio Bursts: Theory and Space Weather Implications

Recent data and theory for type II solar radio bursts are reviewed, focusing on a recent analytic quantitative theory for interplanetary type II bursts. The theory addresses electron reflection and acceleration at the type II shock, formation of electron beams in the foreshock, and generation of Langmuir waves and the type II radiation there. The theory's predictions as functions of the shock and plasma parameters are summarized and discussed in terms of space weather events. The theory is consistent with available data, has explanations for radio-loud/quiet coronal mass ejections (CMEs) and why type IIs are bursty, and can account for empirical correlations between type IIs, CMEs, and interplanetary disturbances. This revised version was published online in August 2006 with corrections to the Cover Date.     

Real-Time Specifications of the Geospace Environment

We report the recent progress in our joint program of real-time mapping of ionospheric electric fields and currents and field-aligned currents through the Geospace Environment Data Analysis System (GEDAS) at the Solar-Terrestrial Environment Laboratory and similar computer systems in the world. Data from individual ground magnetometers as well as from the solar wind are collected by these systems and are used as input for the KRM and AMIE magnetogram-inversion algorithms, which calculate the two-dimensional distribution of the ionospheric parameters. One of the goals of this program is to specify the solar-terrestrial environment in terms of ionospheric processes, providing the scientific community with more than what geomagnetic activity indices and statistical models provide. This revised version was published online in August 2006 with corrections to the Cover Date.     

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。