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.     

跨超、高超声速风洞模型动导数试验技术研究

介绍了气动中心高速所为航空航天飞行器所开展的动导数试验技术研究,主要包括高速大攻角动导数试验技术、再入体模型配平状态动导数试验技术及基于气体轴承的高超声速风洞模型滚转阻尼导数试验技术。阐述了这些试验技术的试验设备及测试系统,给出了典型的试验结果,并进行了分析与讨论。     

利用边条涡抑制Y形进气道流场畸变

已用于飞机外流流场控制的边条涡技术被首次引入内流场的控制,抑制进气道出口流场畸变,改善进发匹配。针对某型飞机的 Y形进气道,有 3对边条涡片被加装在进气道内,与通常的涡流发生器不同的是,这些涡片被设计来控制整个进气道流场而不是仅仅改善局部的附面层。大量的实验结果证实,这种流场控制措施的改善效果显著,某型飞机的 Y形进气道在亚、跨和超声速等各种飞行速度,及不同攻角、侧滑角和开关放气门等飞行条件下,其出口流场畸变均减小,尤其是原流场畸变较大的情况下改善更加明显。     

用集成功放组成的精密功率放大器

介绍了一种用厚膜集成功放加上稳幅电路组成的精密功率放大器，其稳定度、频率响应和波形失真都达到了很高的指标。     

飞机平尾偏转对大迎角动态气动特性的影响

给出了 BJ-1背景机有不同平尾偏角时静态和大振幅俯仰振荡情况下的气动特性。根据风洞实验结果,采用基于三角剖分数据库建模的方法,计算了任意平尾偏角和任意振动频率时的背景机动态气动特性,与实验结果比较表明,提出的有平尾偏角的建模方法能提供任意舵偏时的全机气动特性。在非定常建模的基础上,采用动导数仿真,分析了不同平尾偏角时的动导数,结果表明,水平尾翼偏角主要对零动态阻尼所对应迎角有较大影响,随着舵偏角的增大,该迎角减小。     

H型叶栅通道流计算网格的改进

提出一种壁面正交、尾迹区网格节点分布逐渐均匀化叶栅通道网格生成方法。为了研究壁面处网格正交性对数值计算结果的影响，推导出壁面附近流动参数一阶导数离散误差与网格线交角的数学关系。采用N-S方程分别对平板紊流附面层流和叶栅通道流进行计算分析。结果表明：壁面处网格正交性对附面层内流动计算预测精度影响较大，而对势流区流动影响很小；尾迹区切向网格节点逐渐均匀化分布能更准确计算尾迹区流动。     

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.     

立式风洞设计关键技术探索与实验研究

试验段气流速度快速调节、试验段碟形流场分布、风洞振动与试验段气流脉动的抑制是立式风洞研制的关键技术.本文简介了对这些技术的探索与设计思路,并通过分析φ0.33m立式风洞中进行的一系列性能研究试验结果,得出了相关结论.