EXPERIMENTAL RESEARCH OF THE CONFIGURATION OF WING－TIP DRAG REDUCTION FOR LIGHT AIRCRAFT

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Broadening of Fe X (6374 Å) profiles above the limb in a coronal hole

Profiles of the visible Fe X (6374 Å) coronal emission line as a function of height above the limb were obtained out to 1.16 solar radii in a coronal hole using the NSO/Sacramento Peak Observatory Coronagraph, Universal Spectrograph and a CCD camera. These are the first coronal line profiles obtained as a function of height in a coronal hole from the ground. Analysis of the line widths suggests a large component of nonthermal broadening which increases with height ranging from 40 to 60 km/s, depending upon the assumed temperature or thermal component of the profile.     

高密度栅测应变

将高密度光栅应用于力学参量的测量中。通过测得试件变形前后正交光栅衍射点阵的偏移移量，可逐点得到试件因载荷作用而引起的面内应变、离面位移和刚体传动分量。     

低RCS飞行器外形设计实践

 在鸭式布局的基础上 ,对飞行器各部件及部件间的连接方式进行了外形隐身设计。对初步形成的鸭翼 -翼身融合体改变机身头部形状和立尾配置等进行 RCS优化。给出了飞行器各种状态下的 RCS平均值和迎头± 45°区内的 RCS值。测试结果表明 ,尖头机身、 30°双立尾 (立尾与垂直平面成± 30°角 )的鸭翼 -翼身融合体的 RCS值最小。对 RCS优化后的外形 ,风洞测力试验表明其气动性能也较好 (最大升阻比达到 8,失速迎角超过 2 6°)     

从自动飞行到自主飞行--飞行控制与导航技术发展的转折和面临的挑战

无人机要替代有人驾驶飞机 ,在不确定性环境中执行各类任务 ,必然面临着自主控制的巨大挑战。先进飞行控制和导航技术作为最主要的支撑技术 ,目前只能适应相对结构化任务环境的要求 ,而要解决动态、不确定环境下的自主飞行控制问题尚有很大的差距。当前 ,由自动飞行到自主飞行 ,已发展到了一个大的转折点。本文将从人与机器的关系和人 -机分工及演进的角度阐述作者对这些问题的现状、发展和面临的挑战所进行的系统分析。     

振动尖塔对风洞模拟大气湍流边界层的作用

针对大气边界层风洞模拟中常常出现的湍流度随高度衰减太快的问题，本文尝试了一种新的被动模拟方法——振动尖塔法。该方法主要采用了具有弹性底座的尖塔型旋涡发生器。尖塔群受风洞自由来流驱动，发生随机振动，向下游流场注入了强烈的低频扰动，致使试验区的湍流度、积分尺度和风谱惯性子区的宽度都明显增加，改善了风洞的模拟性能。     

三元收缩段优化设计研究

本文以某低速风洞收缩段为例，对收缩段设计方案的数值计算结果进行了综合分析。文中给出了数值计算结果、分析过程以及典型算例，并给出了该风洞收缩段最佳的气动设计方案，分析了几种常用收缩曲线的特点，同时给出了低速风洞收缩段气动设计的优化过程和可行的方法。结果表明，本文提出的优化设计方法是风洞三元收缩段气动设计较好的有效的气动设计手段。     

直升机机动飞行仿真的气动建模及试验研究

 建立了适用于直升机机动飞行仿真的动力学模型。为了提高模型的真实度,着重通过瞬态操纵实验研究建立了旋翼非定常气动模型;又通过旋翼/ 机身气动干扰试验研究,并运用神经网络技术建立了一种新的机身气动力模型。使用该仿真模型做出的UH260A 直升机仿真计算结果与飞行试验数据符合良好。     

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.