地磁急始年发生数周期特征的小波分析

采用小波分析方法分析了急始年发生数的时间序列的周期特征，并对急始发生数的特征与太阳黑子相对数的特征进行了简要的对照分析，分析结果表明，急始发生数的周期规律与太阳黑子相对数的周期规律是有差异的．还进行了太阳黑子相对数与急始数的相关性，太阳黑子相对数与急始磁暴的相关性研究，分析结果表明它们之间显著相关．还对急始数与急始磁暴致以及其他的一些参数之间的相关性进行了分析，最后对分析结果进行了讨论．     

1989年3月太阳活动引起的强烈磁暴群

本文分析了1989年3月上旬一个太阳超级活动区中多次特大耀斑引起的强磁暴群.联系源耀斑的等级、位置等讨论了磁暴形态特征.随着耀斑活动区位置由东向西旋转,磁暴的形态呈现有规律的变化,充分显示了磁暴形态特征有依赖于耀斑位置的中心子午线效应和东西不对称性.     

Transition region line-shifts in the rebound shock spicule model

Spectral emission lines created in the solar chromosphere — corona transition region show net red-shifts. It has been proposed that this may be the result of the return of spicular material. We simulate a spicule numerically using the rebound shock model and find that the resulting hydrodynamic evolution leads to a perceived up-flow in transition region spectral lines even though the average velocity in the line forming region is directed downward. The explanation for this apparent paradox is found in the correlation between density and velocity in the waves generated by the rebound shock spicule.     

关于天地往返运输系统动力装置

本文对未来天地往返运输系统宜采用的动力装置方案提出一些看法,着重阐明液氧/烃类/液氢三组元推进剂发动机的优点。     

天地往返运输系统空气喷气组合式发动机方案探讨

本文初步探讨了用作天地往返运输系统推进装置的组合发动机,估算了其性能、尺寸、重量以及使用这些发动机时的运载能力。     

跨音压气机确定应力场分析

采用全三维黏性定常、非定常数值模拟技术,对NASA 67第1级的固有非定常流动进行了研究.首先分析了定常流场和非定常时均流场间的差别以及压气机中典型的转、静干涉现象,然后对通道内确定应力的分布规律和转、静交界面确定应力各项的分布特点进行了较为深入的研究,揭示了现有确定应力模型的一些局限性,可为确定应力建模提供一定的指导作用.     

卫星喷气推进系统气密性的保障

本文根据作者多年从事卫星喷气推进系统的设计与试验工作经验,对卫星喷气推进系统气密性保障的重要意义,系统的一般构成情况、气密性指标的确定,系统漏泄的原因和预防,以及常用于卫星喷气推进系统的检漏方法等方面进行了论述.     

Evolution of the Protosolar Nebula and Formation of the Giant Planets

The formation of planetary systems is intimately tied to the question of the evolution of the gas and solid material in the early nebula. Current models of evolution of circumstellar disks are reviewed here with emphasis on the so-called “alpha models” in which angular momentum is transported outward by turbulent viscosity, parameterized by an dimensionless parameter α. A simple 1D model of protoplanetary disks that includes gas and embedded particles is used to introduce key questions on planetesimal formation. This model includes the aerodynamic properties of solid ice and rock grains to calculate their migration and growth. We show that the evolution of the nebula and migration and growth of its solids proceed on timescales that are generally not much longer than the timescale necessary to fully form the star-disk system from the molecular cloud. Contrary to a widely used approach, planet formation therefore can neither be studied in a static nebula nor in a nebula evolving from an arbitrary initial condition. We propose a simple approach to both account for sedimentation from the molecular cloud onto the disk, disk evolution and migration of solids. Giant planets have key roles in the history of the forming Solar System: they formed relatively early, when a significant amount of hydrogen and helium were still present in the nebula, and have a mass that is a sizable fraction of the disk mass at any given time. Their composition is also of interest because when compared to the solar composition, their enrichment in elements other than hydrogen and helium is a witness of sorting processes that occured in the protosolar nebula. We review likely scenarios capable of explaining both the presence of central dense cores in Jupiter, Saturn, Uranus and Neptune and their global composition. This revised version was published online in August 2006 with corrections to the Cover Date.     

电控旋翼气弹动力学建模研究

研究了电控旋翼的气弹动力学建模方法.以有限元旋翼气弹分析程序LORA01为基础,首先给出了一种能计及襟翼移轴补偿影响的时域综合非定常气动力模型,并将伺服襟翼作为额外引入的质量体计入结构动力学模型;之后结合有限元法,根据Hamilton原理导出由广义力表示的带襟翼桨叶非线性运动方程,采用基于Newmark方法的隐式数值积分法对桨叶运动方程进行求解.最后,利用主动控制襟翼旋翼的试验数据对模型进行了比较验证,证明了所建模型的正确性.