The Radio Plasma Imager investigation on the IMAGE spacecraft

Radio plasma imaging uses total reflection of electromagnetic waves from plasmas whose plasma frequencies equal the radio sounding frequency and whose electron density gradients are parallel to the wave normals. The Radio Plasma Imager (RPI) has two orthogonal 500-m long dipole antennas in the spin plane for near omni-directional transmission. The third antenna is a 20-m dipole along the spin axis. Echoes from the magnetopause, plasmasphere and cusp will be received with the three orthogonal antennas, allowing the determination of their angle-of-arrival. Thus it will be possible to create image fragments of the reflecting density structures. The instrument can execute a large variety of programmable measuring options at frequencies between 3 kHz and 3 MHz. Tuning of the transmit antennas provides optimum power transfer from the 10 W transmitter to the antennas. The instrument can operate in three active sounding modes: (1) remote sounding to probe magnetospheric boundaries, (2) local (relaxation) sounding to probe the local plasma frequency and scalar magnetic field, and (3) whistler stimulation sounding. In addition, there is a passive mode to record natural emissions, and to determine the local electron density, the scalar magnetic field, and temperature by using a thermal noise spectroscopy technique.     

Muon Observations

Muon observations are complementary to neutron monitor observations but there are some important differences in the two techniques. Unlike neutron monitors, muon telescope systems use coincidence techniques to obtain directional information about the arriving particle. Neutron monitor observations require simple corrections for pressure variations to compensate for the varying mass of atmospheric absorber over a site. In contrast, muon observations require additional corrections for the positive and negative temperature effects. Muon observations commenced many years before neutron monitors were constructed. Thus, muon data over a larger number of solar cycles is available to study solar modulation on anisotropies and other cosmic ray variations. The solar diurnal and semi-diurnal variations have been studied for many years. Using the techniques of Bieber and Chen it has been possible to derive the radial gradient, parallel mean-free path and symmetric latitude gradient of cosmic rays for rigidities <200 GV. The radial gradient varies with the 11-year solar activity cycle whereas the parallel mean-free path appears to vary with the 22-year solar magnetic cycle. The symmetric latitudinal gradient reverses at each solar polarity reversal. These results are in general agreement with predictions from modulation models. In undertaking these analyses the ratio of the parallel to perpendicular mean-free path must be assumed. There is strong contention in the literature about the correct value to employ but the results are sufficiently robust for this to be, at most, a minor problem. An asymmetric latitude gradient of highly variable nature has been found. These observations do not support current modulation models. Our view of the sidereal variation has undergone a revolution in recent times. Nagashima, Fujimoto and Jacklyn proposed a narrow Tail-In source anisotropy and separate Loss-Cone anisotropy as being responsible for the observed variations. A new analysis technique, more amenable to such structures, was developed by Japanese and Australian researchers. They confirmed the existence of the two anisotropies. However, they found that the Tail-In anisotropy is asymmetric and that both anisotropies had different positions from the prediction. Most 27-day modulations are observed at neutron monitor rigidities but not so readily at higher rigidities. An exception to this is the Isotropic Intensity Wave modulation observed in the early 1980s and again in 1991. This modulation is very strongly related to the heliospheric sector structure and implies a significantly different cosmic ray density on either side of the neutral sheet. The interpretation of most cosmic ray modulation phenomena requires good latitude coverage in both hemispheres. The closure of many muon observatories is a matter of concern. In the northern hemisphere a few new instruments are being constructed and spatial coverage is barely adequate. In the southern hemisphere the situation is far worse with the possibility that within a decade only the Mawson observatory in Antarctica will still be in operation. This revised version was published online in August 2006 with corrections to the Cover Date.     

空间级加成型室温硫化硅橡胶粘结剂的研究

研究了一种新的空间级加成型室温硫化硅橡胶KH—SP—B ,它的特点在于具有低的热真空失重 ,在 12 5℃× 2 4h ,1× 10 - 10 MPa下的热真空失重可小于 0 .3% ;高的粘接强度 ,与金属及聚酰亚胺等的粘结强度可达到 2MPa以上 ;高的热稳定性能 ,分解温度可达 52 4℃ ;优异的低温性能 ,脆性温度为 - 114℃ ;良好的电性能 ,体积电阻率可达 1.3× 10 16 Ω·cm。是一种综合性能优良的空间级室温硫化硅橡胶。     

用推力矢量控制技术改进超声速飞行器空气动力特性

为了提高某超声速飞机的空气动力学效率和机动性能,本文采用低阶的三维板块法和DATCOM半经验公式,在亚声速和超声速条件下,对不同马赫数和迎角情况计算了基本气动外形的飞机空气动力学特性、表面压力分布以及最大升力。此外还开发了一套软件以实现由引进的先进气动操纵面（如鸭翼等）控制的二维推力矢量技术。试验结果表明：气动操纵面结合推力矢量技术能够产生足够的低头力矩,且有能力满足高度机动飞行时的稳定性要求。此外,不论是亚声速还是超声速飞行,气动操纵面均可以提高气动效率5％-6％。     

电视自导引制导武器仿真研究

简述了精确制导武器在现代信息化战争中的重要地位和作用.建立了电视自动寻的制导导弹的完整模型,包括了传感器模型、过载控制模型、自动驾驶仪及导引头模型.通过对全弹道的三维仿真确定了该导弹的毁伤概率,命中精度等评估指标,并分析了各种干扰因素对空地导弹命中精度的影响.仿真验证了所提出模型的正确性,也为实弹打靶提供了有效的辅助决策作用.     

利用几何遗传方法优化前缘翼根延伸的外形以增强飞行器升力系数和机动性

为了提高所选定飞行器模型的机动性,采用了一种标准遗传算法设计前缘翼根延伸(LEX).同时使用一种由三维低阶板方法结合DATCOM方法半经验公式的改进方法预测复杂外形飞行器(机身 机翼 尾翼)的空气动力载荷和最大升力系数.结果表明,在前缘翼根存在的情况下,升力系数在马赫数为0.4～0.8时提升了20.5%～15.3%,在马赫数为1.2时提升了6.8%,在马赫数为0.2～0.95之间升力系数最大值提升了9.5%～15%.在1～5 km的高度亚音速飞行时,其回转率得到了6.6%～8.0%的提升.     

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.     

大攻角流动的非定常特性分析

本文首先通过动态测量手段研究了大攻角流场中的能量成分,分析了各种成分引发的非定常性对大攻角流动的影响。结果表明大攻角流动本身是一种“涡行为”,非定常性对大攻角流动非对称性的影响较弱,影响大攻角流动的本质因素是涡的动力不稳定性对于前体不确定小扰动的响应。