The Medium Energy Instrument on Exosat

The Medium Energy Instrument on EXOSAT, although conceived as the main instrument for occultations, has been made sufficiently versatile to provide a significant advance over previous large area proportional counters when used for individual source studies of timing and spectra. The energy range is 1.2 to 50 keV, with E/E of 0.2 at 6 keV, sufficient to detect iron lines. The effective area of 1800 cm² and narrow field of view (3/4° × 3/4°) make it suitable for the detailed study of sources down to the 0.3 mCrab confusion limit. The unique facility provided by EXOSAT, allowing uninterrupted observations of X-ray sources for periods of up to 80 hours, backed up by a high capacity data link and on-board processing, enables timing studies to be performed over the range from milliseconds to days. Sophisticated background discrimination techniques giving a rejection efficiency of99% will control the background count rate to a suitably low value in the environment of the 200,000 km orbit.     

Scanning Spaceborne Synthetic Aperture Radar with Integrated Radiometer

Spaceborne synthetic aperture radar systems are severely constrained to a narrow swath by ambiguity limitations. Here a vertically scanned-beam synthetic aperture system (SCANSAR) is proposed as a solution to this problem. The potential length of synthetic aperture must be shared between beam positions, so the along-track resolution is poorer; a direct tradeoff exists between resolution and swath width. The length of the real aperture is independently traded against the number of scanning positions. Design curves and equations are presented for spaceborne SCANSARs for altitudes between 400 and 1400 km and inner angles of incidence between 20° and 40°. When the real antenna is approximately square, it may also be used for a microwave radiometer. The combined radiometer and synthetic-aperture (RADISAR) should be useful for those applications where the poorer resolution of the radiometer is useful for some purposes, but the finer resolution of the radar is needed for others.     

重整气爆轰增压燃烧特性分析

为了提高燃气轮机的热效率,提出将化学回热技术（CR）与连续旋转爆轰增压燃烧（CRDPC）技术进行有效结合的思路.通过实验研究与数值研究的方法分别考察了不同的甲烷蒸汽重整方案对热回收的影响、重整气的增压燃烧流场特性及燃烧室性能等.结果表明:并列协同催化甲烷蒸汽重整方案具有最佳的重整性能,甲烷转化率和总焓增加率分别达到46.51%和25.28%;重整气组分的差异对爆轰波系流场结构影响较小,但是氢气质量分数的增加可以提高爆轰波传播速度,也会加剧新鲜预混气与上一轮爆轰产物的接触间断处的提前燃烧;在总压相同且重整气与空气以化学当量比进行预混的前提下,重整气中氢气质量分数增加1.1%左右时,预混气入口比质量流量降低约4.5%,但连续旋转爆轰燃烧室增压比降低约6.0%,这主要是接触间断处的提前燃烧造成的.      

肼混合物胶体推进剂的热分解特性研究

为了评估肼混合物胶体推进剂的热安全性,采用差示扫描量热仪(DSC)和绝热加速量热仪(ARC),对肼混合物胶体推进剂的热分解特性进行了研究。DSC的实验结果表明,在2,5,10和20K·min-1四种升温速率下推进剂的初始热分解温度分别为185.73,227.20,230.37和245.19℃;根据DSC的试验结果,利用Kissinger法计算得到热分解活化能为181.80k J·mol-1。在ARC实验中,肼混合物胶体推进剂在理想绝热条件下的初始分解温度为180.58℃,最大温升速率达到0.6237°C·min-1,绝热温升为227.92℃,最高温度为408.50℃,计算得到其热分解活化能为121.77k J·mol-1。比较DSC与ARC的试验结果,两者基本一致;热分析试验中推进剂先经历相变吸热过程,再进行分解放热。     

SA一方程湍流模型参数影响分析与辨识

SA(Spalart-Allmaras)一方程湍流模型是目前工程湍流计算中主要采用的湍流模型之一。首先,针对某典型战斗机的小攻角、中等攻角、大攻角流动工况,利用均匀试验设计方法分析SA一方程模型中8个参数取值对上述工况下飞机升力和阻力系数计算结果的影响规律;然后,建立工程湍流模型参数的辨识方法,并将其用于该战斗机大攻角工况下湍流模型参数cb1值的辨识调整。结果表明:不同工况下,湍流模型参数对计算结果的影响规律不同;在附着流状态下,对升力和阻力影响较大的参数是cv1和cb1;在中等攻角和较大攻角下,对升力和阻力影响较大的参数是cb1;适当减小参数cb1的取值后,升力和阻力系数的计算结果有较明显的改善,这可能与飞机大攻角分离流场中涡粘系数和剪切应力的发展与自由剪切流存在一定差异有关。     

考虑控制系统故障的重复使用运载器轨迹优化

传统的重复使用运载器的制导系统与控制系统的设计是分开进行的。当运载器出现故障时,需要进行轨迹和控制的重构,故障下气动特性和配平能力的变化使得重构后的制导系统与控制系统难以良好匹配。考虑到控制系统对轨迹设计和优化的影响,通过将三自由度轨迹优化与多舵面控制分配结合,提出一种考虑控制舵面气动力和故障的重复使用运载器轨迹优化方法。仿真结果表明,多舵面控制分配算法可以将运载器故障下的配平能力转化为轨迹优化的约束条件,从而避免了传统三自由度轨迹优化方法结果无法被控制系统跟踪的可能性,并为制导与控制一体化设计提供参考依据。     

超声速内埋武器不同分离方式分析

为给高空高速无人机内埋武器分离方式的选择提供权衡依据,建立了弹舱及弹体模型,采用chimera嵌套网格方法与Menter SST k-ω湍流模式,对舱内重力投放、舱内弹射投放及舱外重力投放三种内埋武器分离方式在高空高速条件下的内埋武器分离过程进行了仿真分析,对比了三种分离方式分离过程的流场特性与弹体运动参数。结果表明,在Ma=3.7,高度为2.5 km的条件下,舱内弹射投放与舱内重力投放能够使内埋武器安全分离,舱外重力投放在高空高速条件下无法完成内埋武器的安全分离,弹体无法快速下落并伴有大幅振荡,威胁无人机的飞行安全。     

连续旋转爆轰燃烧室增压特性的数值研究

为了分析爆轰燃烧室几何尺寸对增压特性的影响,利用二维欧拉方程数值研究了当量H2/Air在连续旋转爆轰燃烧室中的燃烧流场情况。研究表明:在准稳定状态下爆轰燃烧流场特征参数随时间呈周期性振荡,且其振幅保持不变;横波及局部爆炸波的存在是爆轰波后侧附近总压沿x轴呈现波动变化的主要原因;影响连续旋转爆轰燃烧室增压特性的直接因素为斜激波的高度及爆轰波强度,减少轴向尺寸或增加周向尺寸可增强其增压特性。连续旋转爆轰燃烧室的增压比高达2.52,与传统的燃烧室相比,大大提高了燃气的做功能力。     

Understanding Interplanetary Coronal Mass Ejection Signatures

While interplanetary coronal mass ejections (ICMEs) are understood to be the heliospheric counterparts of CMEs, with signatures undeniably linked to the CME process, the variability of these signatures and questions about mapping to observed CME features raise issues that remain on the cutting edge of ICME research. These issues are discussed in the context of traditional understanding, and recent results using innovative analysis techniques are reviewed.     

Coronal Mass Ejections: Overview of Observations

We survey the subject of Coronal Mass Ejections (CMEs), emphasizing knowledge available prior to about 2003, as a synopsis of the phenomenology and its interpretation.