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.     

风挡防冰表面温度场计算

在研究国内外有关资料的基础上，采用了量纲分析的方法，建立了风挡外表面温度场的计算模型。回避了对自由流与射流相互干扰这一复杂问题的研究，同时对该计算模型进行了验证，并开发了相应的计算程序。该问题的解决，填补了国内在该领域中的空白。     

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.     

直升机动力学中参数振动问题的数值解法

 参数振动问题是直升机的基本动力学问题之一,旋翼桨叶的挥舞弯曲微分方程和摆振弯曲微分方程都是复杂的参数振动问题,在许多计论直升机旋翼动力学的论著中~[1-4],有的虽然推导了复尽杂的参数振动方程,却没有提到求解的方法,有的对此根本没有论及.本文旨在讨论参数问题的数值解法.     

壁压法在非矩形风洞中的应用

 解决大攻角洞壁干扰修正的壁压法,是利用一定数量固定位置和形状的线源和线涡来模拟风洞内模型的堵塞效应和升力效应。矩形风洞实验段边界对绕模型流动的影响,可用两个方向有限层的镜像线源和线涡来代替,并利用在风洞上下壁和侧壁上测压点处测量所得     

Experimental Aspects of Mid-Frequency Pulsations (f≈10–100 mHz) in the Southern Polar Cap

We review the results obtained in the frequency range of Pc3 (22-100 mHz) and Pc4 (7-22 mHz) pulsations at Italian Antarctic stations in the southern polar cap (“Mario Zucchelli”, at Terra Nova Bay, TNB, 80^˚.S; “Concordia”, the Italian/French base at Dome C, DMC, 89^˚.S). The absence of a midnight enhancement in the pulsation power suggests a negligible substorm influence at extreme latitudes, while the sharp noon enhancement, which appears only at TNB, is determined by the closer proximity of the station to cusp related phenomena. The relationship between the frequency of the band-limited signals and the interplanetary magnetic field strength, the cone angle influence, and the higher correlation of the Pc3 power with the solar wind speed in the morning hours suggest a global scenario in which upstream waves would be mainly responsible for the mid-frequency activity in the polar cap. However, the polarization pattern is odd with respect to the predictions for tailward propagating modes.     

翼型风洞侧壁干扰的数值模拟研究

运用Navier-Stokes数值模拟对翼型模拟试验对风洞侧壁干扰进行模拟，将简单代数湍流模型扩展用于机翼／风洞侧壁结合区流动，分析了风洞实验侧壁干扰问题的形成机理和影响翼型实验侧壁干扰的各种因素，如翼型展长、风洞侧壁边界层厚度及侧壁边界层抽吸等，对实验结果的影响，得出了一些有用的结论。计算格式空间采用中心有限体积离散，时间采用多步Runge-Kutta时间步长格式进行积分。计算结果证明了该方法的可行性和优越性。     

利用林胶茶人工群落减弱台风对橡胶林破坏机理的风洞模拟试验研究

本文研究台风登陆时（中性大层结）胶茶人工群落内部及上部风速的变化，湍流结构的变化及阻力的变化，来分析判断基减弱台风破坏的机理，评定最佳防风效果的林胶茶人工群落方案。试验研究证明台风吹向胶茶人工群落，台风越过和穿过林带，由于气流与树冠，枝叶的冲击与摩作用，使台风风速大大降低，使动能大大损失，使原来动能强和湍流弱的较大尺度旋涡的台风，变成旋涡尺度较小的动能弱湍流强的湍流，湍流能量的增强反映了风速递减率     

街道峡谷湍流流动的风洞试验与数值计算

在１：２５０的风洞模型上,测量街道峡谷的平均流速,湍流度等参数,分析了街道峡谷内的湍流流动状态,探讨了屋顶来流风在街道峡谷内产生复杂流场的主要特征,并用三维湍流流模型对风洞试验模型进行了数值计算,试验和计算结果为研究街道峡谷风环境以及街道峡谷的传热传质过程提供了基础。     

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.