直升机六自由度仿真研究

建立了直升机剐体运动的六自由度仿真模型。用试飞数据进行参数识别，建立了气动导数数据库并以此计算气动力；将仿真结果与试飞结果对比，并进行了直升机机动飞行仿真计算。结果表明：六自由度仿真模型能够得到较好的仿真结果。     

用Newton子迭代方法计算前飞旋翼粘性绕流

通过求解Navier-Stokes方程数值模拟了直升机旋翼前飞非定常流场，为了同时保证计算的时间精确性和计算效率，时间推进格式采用了双时间推进方法，在该方法中，子迭代过程由十分高效的LU-SSOR方法完成，且使子迭代过程成为Newton子迭代，空间上应用中心平均的有限体积法进行离散，为了模拟前飞桨时间的相对运动，网格布局采用了运动嵌套网格方法，应用本文方法对-悬停流场进行了数值计算，计算结果与实验吻合较好，尽管缺乏实验数据的验证，对-有升力前飞状态的数值模拟结果是可信的。     

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。     

Modeling of dynamic evolution of coronal loops

Parameters of expanding magnetic loops and arches and of mass flows generated by them in the corona have been computed in a 1D two-fluid approximation. Two possible trigger mechanisms of the coronal transients have been considered: (i) sudden increase of the background magnetic field strength, and (ii) heating and compression plasma inside these magnetic structures. We discuss the formation of shock waves and their dependence on dynamics and geometry of the magnetic structures.     

复合材料动模量振动测定方法的研究

 本文采用Timoshenko梁理论,首次导出了悬臂梁和自由-自由梁自由端具有附加质量的特征方程,并进而讨论了多种因素对动模量计算值的影响。此外还提出了用弯曲振动确定剪切动模量G_(12)的一般方法。最后进行了实例分析和讨论。     

GH4169高温合金惯性摩擦焊接头动态再结晶过程

当温度、应变、应变速率达到一定条件时 ,GH4 16 9镍基高温合金在惯性摩擦焊接过程中易发生动态再结晶。本文研究结果表明 ,由于GH4 16 9合金惯性摩擦焊接时间很短 ,动态再结晶进行得相当充分 ,而动态回复不足 ,在动态再结晶的过程中还可以看到有些结晶过程还处于形核阶段 ,这是惯性摩擦焊接头产生细晶乃至超细晶的根本原因     

基于Web services的软件集成技术研究

本文对Web services技术的基本特点进行了探讨,并应用ENOVIA Web service和SOAP的开放特性,设计了直升机设计数据在全生命周期管理系统与第三方软件系统之间交换的接口,解决了设计信息跨平台通讯和系统的灵活集成问题。     

Solar Gamma-Ray Spectroscopy

Interactions of ions accelerated in solar flares produce gamma-ray lines and continuum and neutrons. These emissions contain a rich set of observables that provides information about both the accelerated ions and the environment where the ions are transported and interact. Ion interactions with the various nuclei present in the ambient medium produce gamma-ray lines at unique energies. How abundance information is extracted from the measurements is discussed and results from analyses of a number of solar flares are presented. The analyses indicate that the composition of the ambient gas where the ions interact (typically at chromospheric densities) is different from that of the photosphere and more like the composition of the corona, exhibiting low-FIP elemental enhancements that may vary from flare to flare. Evidence for increased Ne/O and the photospheric ³He abundance is also discussed.     

The Local Bubble and Interstellar Material Near the Sun

The properties of interstellar matter at the Sun are regulated by our location with respect to a void in the local matter distribution, known as the Local Bubble. The Local Bubble (LB) is bounded by associations of massive stars and fossil supernovae that have disrupted dense interstellar matter (ISM), driving low density intermediate velocity ISM into the void. The Sun appears to be located in one of these flows of low density material. This nearby interstellar matter, dubbed the Local Fluff, has a bulk velocity of ∼19 km s⁻¹ in the local standard of rest. The flow is coming from the direction of the gas and dust ring formed where the Loop I supernova remnant merges into the LB. Optical polarization data suggest that the local interstellar magnetic field lines are draped over the heliosphere. A longstanding discrepancy between the high thermal pressure of plasma filling the LB and low thermal pressures in the embedded Local Fluff cloudlets is partially mitigated when the ram pressure component parallel to the cloudlet flow direction is included.     

Stellar flares

Radio and X-ray observations of stellar flares provide the most direct probes of energy relaase particle acceleration, and energy transport on stars other than the Sun. In this review, the observational basis for our understanding of the flare phenomenon on other stars is briefly described and outstanding interpretive and theoretical issues are discussed. I shall confine my attention to objects which are solar-like, to the extent that they possess deep convective envelopes and display activity which is presumed to be magnetic in origin. These include pre-main sequence objects, classical flare stars, and close binaries. Future directions are briefly discussed.