转轴位置对俯仰动态特性的影响

研究了转轴位置对机翼、机身和三个组合体上翼面的动态特性的影响，对于机翼和机身，当转轴位置后移时其动态迟滞效应更为强烈。当翼面处于转轴之前，上仰时会出现更为的动态迟滞效应。因此鸭翼达到失速状态较晚。而当翼面处于转轴之后时，如尾翼，将会更早地出现动失速，转轴位置对动态迟滞特性的影响可以认为主要是由于俯仰运动时的动态洗流影响所导致的实际有效迎角的变化。由此影响了动态分离涡及其发展。     

计算跨声速机翼尾涡流自适应区域方法

本文利用自适应区域方法调节机翼后每个Ｔｒｅｆｆｔｚ平面上的计算域，使得尾涡对这个计算域边界的影响足够小，从而提高了计算的精度和时间。考虑到间断面的影响，在尾涡面上引入有旋项对流场进行计算。椭圆载荷机翼计算表明本文计算结果与经典Ｂｅｔｚ理论一致。用本文方法对某轰炸机进行了计算，计算结果已用于预计其实际飞行的尾涡面。     

用三维欧拉方程计算机身与机翼绕流

本文用Jameson的三维欧拉方程有限体积法、四步Runge-Kutta时间推进格式,计算机身和大后掠细长机翼的三维可压缩绕流。对钝头机身,用C-O型网格;尖头机身与大后掠细长机翼用H-O型网格。本文介绍钝头旋成体、带座舱前机身和三角翼绕流的计算结果,显示流场等值M线分布,计算压强系数分布与实验比较,以及三角翼大迎角分离涡等。由于用了隐式残值光顺等加速收敛措施,有效地减少推进步数,节省机时。     

面向设计的飞机翼面结构有限元自动建模技术

提出一种新的飞机翼面结构分析和优化的建模技术。引入“构件属性”的概念，利用“网状”数据结构来实施管理，并将图形用户界面（GUI）技术与CAD中的基本绘图功能相结合，从而形成具有领域特色的新一代快速和在一定条件下的自动建模系统。建模举例表明：此系统操作简单、使用方便、遵循结构分析与优化建模的专业做法。     

连翼布局飞机及探测无人机研究进展

在收集、整理、分析国外连翼布局飞机研究资料的基础上,介绍了国外连翼布局飞机的研究历程和设计特点;特别是基于近年来对未来战场信息情报、监视、侦察任务的需求,介绍了连翼布局探测无人机这一新的作战概念和装备技术的研究进展情况。     

用欧拉方程计算机翼与翼身组合体绕流

本文用保角转绘加剪切变换生成三维机翼与翼身组合体Ｃ－Ｈ型网格，并在这类网格拓扑上，用有限体积法研制出可供分析机翼与翼身组合体绕流的三维欧拉方程计算程序。本方法的特色是改进了机翼表面网格点的分布，使机翼后缘与网格线一致；采用了当量机身，使机岙表面到对称面光滑过渡；嵌入了边界层粘性修正。改善了计算结果。数值计算表明，对粘性影响较大的超临界绕流，边界层修正效果显著。     

Solar Irradiance Variability Since 1978

Since November 1978 a set of total solar irradiance (TSI) measurements from space is available, yielding a time series of more than 25 years. Presently, there are three TSI composites available, called PMOD, ACRIM and IRMB, which are all constructed from the same original data, but use different procedures to correct for sensitivity changes. The PMOD composite is the only one which also corrects the early HF data for degradation. The results from the detailed analysis of the VIRGO radiometry allow a good understanding of the effects influencing the long-term behaviour of classical radiometers in space. Thus, a re-analysis of the behaviour of HF/NIMBUS-7 and ACRIM-I/SMM was indicated. For the former the situation is complicated by the fact that there are no in-flight means to determine changes due to exposure to solar radiation by comparison with a less exposed radiometer on the same spacecraft. The geometry and optical property of the cavity of HF is, however, very similar to the PMO6-type radiometers, so the behaviour of the PMO6V radiometers on VIRGO can be used as a model. ACRIM-I had to be revised mainly due to a henceforth undetected early increase and a more detailed analysis of its degradation. The results are not only important for solar radiometry from space, but they also provide a more reliable TSI during cycle 21. The differences between the revised PMOD composite and the ACRIM and IRMB are discussed by comparison with a TSI reconstruction from Kitt-Peak magnetograms. As the PMOD composite is the only one which has reliable data for cycle 21, the behaviour of the three solar cycles can now be compared and the similarities and differences discussed.     

What do Cosmogenic Isotopes Tell us About Past Solar Forcing of Climate?

In paleoclimate studies, cosmogenic isotopes are frequently used as proxy indicators of past variations in solar irradiance on centennial and millennial timescales. These isotopes are spallation products of galactic cosmic rays (GCRs) impacting Earth's atmosphere, which are deposited and stored in terrestrial reservoirs such as ice sheets, ocean sediments and tree trunks. On timescales shorter than the variations in the geomagnetic field, they are modulated by the heliosphere and thus they are, strictly speaking, an index of heliospheric variability rather than one of solar variability. Strong evidence of climate variations associated with the production (as opposed to the deposition) of these isotopes is emerging. This raises a vital question: do cosmic rays have a direct influence on climate or are they a good proxy indicator for another factor that does (such as the total or spectral solar irradiance)? The former possibility raises further questions about the possible growth of air ions generated by cosmic rays into cloud condensation nuclei and/or the modulation of the global thunderstorm electric circuit. The latter possibility requires new understanding about the required relationship between the heliospheric magnetic fields that scatter cosmic rays and the photospheric magnetic fields which modulate solar irradiance.     

Type II Solar Radio Bursts: Theory and Space Weather Implications

Recent data and theory for type II solar radio bursts are reviewed, focusing on a recent analytic quantitative theory for interplanetary type II bursts. The theory addresses electron reflection and acceleration at the type II shock, formation of electron beams in the foreshock, and generation of Langmuir waves and the type II radiation there. The theory's predictions as functions of the shock and plasma parameters are summarized and discussed in terms of space weather events. The theory is consistent with available data, has explanations for radio-loud/quiet coronal mass ejections (CMEs) and why type IIs are bursty, and can account for empirical correlations between type IIs, CMEs, and interplanetary disturbances. This revised version was published online in August 2006 with corrections to the Cover Date.     

High-Frequency Radio Signatures of Solar Eruptive Flares

Several examples of the radio emission of eruptive solar flares with high-frequency slowly drifting structures and type II bursts are presented. Relationships of these radio bursts with eruptive phenomena such as soft X-ray plasmoid ejection and shock formation are shown. Possible underlying physical processes are discussed in the framework of the plasmoid ejection model of eruptive solar flares. On the other hand, it is shown that these radio bursts can be considered as radio signatures of eruptive solar flares and thus used for the prediction of heliospheric effects. This revised version was published online in August 2006 with corrections to the Cover Date.