复合材料飞机结构验证试验载荷放大系数法

载荷放大系数法的基本原理是将给定载荷（谱）下的结构Ｂ基准寿命验证试验转化为给定Ｂ基准寿命下的结构剩余强度验证试验，载荷放大系数可由理论推导方法和试验方法确定，讨论了复合材料飞机结构全尺寸验证试验采用载荷放大系数法的原因，前提条件、１．１５载荷放大系数的确定和应用的局限性等问题。     

YBCO系超导块材平均粒径对双孔RF－SQUID噪声影响

对不同粒径超导块材的双孔ＲＦ－ＳＱＵＩＤ的噪声水平研究表明，ＹＢＣＯ超导块材的晶粒粒径与双孔ＲＦ－ＳＱＵＩＤ的噪声大小呈Ｕ形关系．在１５～２５μｍ时，噪声水平很低，小于２．０×１０－３φ０／Ｈｚ；反之，噪声水平偏高．     

复合材料层合板开口补强研究

对大开口复合材料层合板（包括拉伸板和剪切板）不同补强型式进行了实验和计算研究，有限元计算与实验结果吻合较好，研究表明，插层补强优于面外补强，对称补强优于非对称补强，非对称补强和凹陷板的偏弯影响很大，凹陷板强度甚致低于未补强板。     

三维编织复合材料强度的数值预报

在实验研究和有限元分析的基础上,提出了一种经验性强度失效判据,并利用刚度预报的模型和有限元分析的结果,进一步提出了强度预报的方法.强度计算的结果表明: 预测值与拉伸实验的结果基本相符.     

复合材料层合结构整体┐局部有限元素法

提出一个精确分析复合材料层合结构应力的整体－局部有限元素法．首先，采用分区直线模型的子单元法，计算整个层合结构的位移和应力．然后，在应力计算精度要求较高的局部区域内，以子单元法计算所得节点位移为基础，以应力参数为基本未知量，利用修正余能原理，进一步精确分析该局部区域的应力．计算表明，该方法对于复合材料层合结构的应力有很高的计算精度     

DCB试样应力强度因子的一个改进公式

利用能量释放率方法与计及剪切变形的工程梁理论导出了一个计及根部变形效庆的ＤＣＢ试样应力强度因子的便于应用的改进型公式，并对原有不计根部变形效应的公式精度进行了评价。     

极大似然法测定p—S—N曲线的置信度

对极大似然法测定的Ｐ－Ｓ－Ｎ赋予置信度，提出了极大似然法珠Ｐ－Ｓ－Ｎ曲线的置信限曲线公式，通过该公式确定的Ｐ－Ｓ－Ｎ能使估算的疲劳寿命具有置信度一给出了单点法测定出构件Ｐ－Ｓ－Ｎ的数据自理。     

关于北斗卫星导航系统的被动式定位算法比较研究

我国北斗卫星导航系统空间卫星共有2或3颗,无法单独满足被动导航定位的要求．针对这种卫星稀少的情况提出了3种被动式定位算法: 2星定位算法、 3星3参数定位算法和3星4参数定位算法, 这些算法分别采用气压测高方法增加观测数据和采用数学模型描述接收机钟差的方法减少定位方程求解的未知数;探讨了北斗卫星导航系统备份星的可用性和对导航定位精度的贡献;还提出了准差分修正技术,提高了定位精度．实验证明, 3种算法都取得了100m以内的定位结果,可以满足一般用户定位需求．     

Study of correlations between waves and particle fluxes measured on board the DEMETER satellite

The topic of relativistic electron dynamics in the outer radiation belt has received considerable attention for many years. Nevertheless, the problem of understanding the physical phenomenon involved is far from being resolved. In this paper, we use DEMETER observations to examine the variations of the energetic electron fluxes and ELF/VLF wave intensities in the inner magnetosphere during the intense 8 November 2004 magnetic storm. Electron flux spectra and associated wave intensity spectra are analysed throughout the magnetic storm and common characteristics or differences to other storm events are retained. The overall objective of this study is to identify and derive parameters that are relevant for particle flux modelling; the time constant characterizing the persistent decay after particle enhancement was found to be one of these important model parameters.The analysis of the 8 November 2004 event reveals that for L-shell parameter higher than 4, an electron flux dropout is observed during the storm’s main phase for electrons in the energy range 0.1–1 MeV, as has been reported from other measurements. Characteristic wave spectra accompanying this phase are analysed. They show a typical enhancement in the frequency range 0.3–10 kHz at onset for all L-shell values under consideration (2 < L < 5). During the first stage of the recovery phase, the electron fluxes are increased to a level higher than the pre-storm level, whereas the level of wave intensity in the frequency range observed below 300 Hz is at its highest. In the second stage, the particle flux decrease goes hand in hand with a global wave activity decline, the relaxation time of the latter being smaller than the former’s one. In some other cases, long-lasting electron enhancement associated with constant wave activity has been observed during this latter stage. For the above mentioned storm, while at low L values the decay time constants are higher for low energy electrons than for high energy electrons, this order is reversed at high L values. At about L = 3.6 the time constant is independent of electron energy.     

Orbital phase spectroscopy of X-ray pulsars to study the stellar wind of the companion

High Mass X-ray Binary Pulsars (HMXBP), in which the companion star is a source of supersonic stellar wind, provide a laboratory to probe the velocity and density profile of such winds. Here, we have measured the variation of the absorption column density along with other spectral parameters over the binary orbit for two HMXBP in elliptical orbits, as observed with the Rossi X-ray Timing Explorer (RXTE) and the BeppoSAX satellites. A spherically symmetric wind profile was used as a model to compare the observed column density variations. In 4U 1538-52, we find the model corroborating the observations; whereas in GX 301-2, the stellar wind appears to be very clumpy and a smooth symmetric wind model seems to be inadequate in explaining the variation in column density.