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.     

真空羽流逆流污染的理论计算

针对普遍关注的羽流逆流污染问题,讨论了喷管出口背部位置受到的回流分子撞击热污染和分子沉积问题,从分子运动论和统计力学出发编制了计算程序,对不同的算例进行了计算,得到符合规律的结果,为火箭发动机设计和科学试验提供了理论依据。     

逆升压电子设备冷却系统控制方案的研究

分析了目前国内一些飞机基于三点温度控制方案的逆升压电子设备冷却系统的缺陷 ,提出了一种新的系统控制方案 ,即基于飞行速度和高度的逆升压电子设备冷却系统的控制方案。这一方案不需要人工干预 ,可实现全自动化。     

CS-01高空台推力测量和校准装置研制

推力是涡喷涡扇发动机高空模拟试验的重要测量参数之一。CS－01高空台原推力测量采用杠杆、砝码、测力秤系统，现采用原位校准，液压加载、应变式推力传感器来测量和校准，从而消除了“高度差”的影响，降低了稳态推力测量系统的测量不确定度。     

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.     

应用于翼型绕流的线性/非线性湍流模式的研究

本文选取了四个线性湍流模式、四个非线性涡粘性湍流模式和一个显式代数应力模式对绕翼型的不可压缩分离流动进行了数值模拟.因计算鲁棒性的需要,其中部分模式在壁面附近耦合了一方程模式.通过与实验结果的比较,对翼型在大攻角情况下流动产生分离的气动特性进行了评估.计算结果表明,非线性模式能够较好地反映湍流的各向异性和曲率影响.     

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。