应力波天平在国内激波风洞上的应用

介绍了应力波天平的特点、原理,通过应力波天平设计、制作、校准、试验、数据处理等方面在中国空气动力研究与发展中心φ0.6m激波风洞上的应用情况,指出有必要在国内激波风洞上更进一步地开展应力波天平测力技术.     

双立尾/三角翼布局的立尾抖振研究

在北航的风洞中进行了双立尾-三角翼布局的立尾抖振实验,目的是研究立尾抖振产生的原因.主要采用了激光测振仪测立尾加速度和动态压力传感器测立尾表面的动态压力的实验方法.实验结果表明在旋涡破裂以后,立尾上就会产生强烈的抖振.抖振是由立尾上表面压力的周期性脉动造成的.对机翼和立尾表面的压力频谱分析表明,立尾上的压力脉动来源于机翼前旋涡破裂流中的螺旋波.对于本实验使用的模型来说,当机翼迎角α=0°~20°范围,由于流动是附着流和涡流,所以立尾没有明显抖振;当机翼迎角在α=20°~56°范围,立尾处在破裂涡流的范围,立尾抖振明显,并且抖振强度在35°~50°之间达到最大.因此,三角翼破裂涡流中的螺旋波正是双立尾产生抖振的主要原因.     

大迎角试验数据精度及影响因素分析

着重分析了粗糙带、偏航角β、模型抖动以及滤波频率、采样时间和样本长度等因素对于大迎角试验数据精度的影响.结果认为:常规试验采用的滤波频率会导致关键气动信息的丢失,滤波频率的选取尤为重要;弯刀系统的横向刚度是影响大迎角数据精度的一个重要因素,试验中如何降低其横向刚度的影响是一难点.     

Four-peak longitudinal distribution of the equatorial plasma bubbles observed in the topside ionosphere: Possible troposphere tide influence

In this paper we consider an idea of the troposphere tide influence on the character of the longitudinal variations in the distribution of the equatorial plasma bubbles (EPBs) observed in the topside ionosphere. For this purpose, the obtained EPB longitudinal patterns were compared with the thermosphere and ionosphere characteristics having the prominent “wave-like” longitudinal structures with wave number 4, which are uniquely associated with the influence of the troposphere DE3 tides. The characteristics of the equatorial mass density anomaly (EMA), equatorial ionization anomaly (EIA), zonal wind and pre-reversal E?×?B drift enhancement (PRE) were used for comparison. The equinox seasons during high solar activity were under consideration. It was obtained that the longitudinal patterns of the EMA and zonal wind show the surprising similarity with the EPB distributions (R???0.8, R???0.72). On the other hand, the resemblance with the ionosphere characteristics (EIA, PRE) is rather faint (R???0.37, R???0.12). It was shown that the thermosphere zonal winds are the most possible transfer mediator of the troposphere DE3 tide influence. The most successful moment for the transfer of the troposphere DE3 tide energy takes place in the beginning of the EPB production, namely, during the seed perturbation development.     

液体运载火箭低温动力系统注气式循环预冷过程的AMESim仿真研究

讨论了液体运载火箭低温动力系统起动前预冷的必要性和循环预冷方案的优缺点,分析了注气式循环预冷的基本原理和影响因素,建立并根据试验数据验证了基于AMESim的注气式循环预冷仿真模型。对不同工况液体运载火箭低温动力系统注气式循环预冷过程进行研究,部分工况获得了与文献试验数据较为一致的规律,并对注气式循环预冷过程伴随的增压下注入气体对贮箱气枕的影响、变过载对系统循环特性的影响和注入气体在贮箱与管路内行为特性等问题进行了分析与讨论。     

空气动力二阶核函数辨识方法

采用截断三阶Volterra级数模型来研究空气动力二阶核函数的辨识问题,选取一簇正交化的切比雪夫多项式对二阶核函数进行参数化处理,并将非参数辨识问题转化成参数辨识问题。相比于其他方法,本文模型能有效降低对激励信号幅值的敏感程度,保证辨识出的核函数具有较好的保真度;只针对三阶Volterra降阶模型中的一阶、二阶核函数进行辨识,即可提升原系统一阶、二阶核函数的辨识精度,却不会显著增加辨识过程的工作量;参数化辨识方法属于整体性辨识,根据已有的部分数据对(输入、输出数据)就能完成系统辨识,且能达到较好的辨识精度,从而有效地减少了执行计算流体力学(CFD)代码程序的总次数,节约了大量的时间成本。算例表明,与目前流行的非参数化方法相比,本文提出的切比雪夫函数辨识方法,精度上达到预期要求,辨识过程消耗的CFD总时间量至少可降低一个数量级。     

The quiescent spectrum of 2S1636-536

During the EXOSAT observation of 2S1636-536 in July 1983 the quiescent flux was observed to brighten from 1.7×10 ^-9 ergs/cm. ² /sec to 2.6×10^-9 ergs/cm. ² /sec, this increase being accompanied by a decrease in effective temperature. Further analysis of the spectrum reveals that the best fit is a power law with an index which increases from -1.75 to-2.1 while the source brightens; there is some evidence for an upper cut off. This spectrum is interpreted as the result of soft photons from the neutron star surface which are Comptonised in a hot plasma cloud surrounding the neutron star (neutron star corona). The increasing spectral index is seen as the result of Compton cooling of the corona as the output of quiescent flux rises in response to an increasing accretion rate.     

Composition,structure and properties of Venus rocks

Physical and mechanical properties as well as chemical and mineral composition of Venus rocks are discussed on the basic of the data obtained by ground-based radar observations and the experiments in situ.     

The Venus ionosphere

Physical properties of the Venus ionosphere obtained by experiments on the US Pioneer Venus and the Soviet Venera missions are presented in the form of models suitable for inclusion in the Venus International Reference Atmosphere. The models comprise electron density (from 120 km), electron and ion temperatures, and relative ion abundance in the altitude range from 150 km to 1000 km for solar zenith angles from 0° to 180°. In addition, information on ion transport velocities, ionopause altitudes, and magnetic field characteristics of the Venus ionosphere, are presented in tabular or graphical form. Also discussed is the solar control of the physical properties of the Venus ionosphere.