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141.
飞船返回舱再入阶段高超声速六分量测力试验研究 总被引:3,自引:0,他引:3
介绍了在气动中心超高速所激波风洞中进行的飞船返回舱再入阶段高超声速六分量测力试验研究以及马赫数、雷诺数变化对返回舱外形纵向三分量气动特性的影响研究。在试验方案和天平设计中提出和采用了“5 l”方案,即五分量主天平和单分量滚转力矩天平实现六分量测量,模型分段连接使大轴向力对小滚转力矩测量的干扰降至最低。为考核该方案的可行性,还进行了一系列验证性试验,如对比性试验和缝隙影响试验,试验研究结果表明:采用该方案是可行的,成功地测量出了返回舱模型上的小滚转力矩。 相似文献
142.
三元收缩段优化设计研究 总被引:18,自引:0,他引:18
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。 相似文献
143.
Kamide Y. Kihn E.A. Ridley A.J. Cliver E.W. Kadowaki Y. 《Space Science Reviews》2003,107(1-2):307-316
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. 相似文献
144.
Alexeev Igor I. Belenkaya Elena S. Bobrovnikov Sergey Yu. Kalegaev Vladimir V. 《Space Science Reviews》2003,107(1-2):7-26
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. 相似文献
145.
146.
利用边条涡抑制Y形进气道流场畸变 总被引:1,自引:0,他引:1
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。 相似文献
147.
148.
J. C. Raymond 《Space Science Reviews》1999,87(1-2):55-66
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. 相似文献
149.
J. L. Kohl S. Fineschi R. Esser A. Ciaravella S. R. Cranmer L. D. Gardner R. Suleiman G. Noci A. Modigliani 《Space Science Reviews》1999,87(1-2):233-236
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. 相似文献
150.