论社会主义市场经济条件下的按劳分配

我国现阶段实行的按唠分配不是马克思原意的按劳分配，而是按社会必要劳动时间分配，是按劳分配原则在社会主义市场经济条件下的转化形式。按社会必要劳动时间分配的实质是按生产要素分配。     

The Role of Magnetic Reconnection in CME Acceleration

Observations carried out from the coronagraphs on board space missions (LASCO/SOHO, Solar Maximum and Skylab) and ground-based facilities (HAO/Mauna Loa Observatory) show that coronal mass ejections (CMEs) can be classified into two classes based on their kinematics evolution. These two classes of CMEs are so-called fast and slow CMEs. The fast CME starts with a high initial speed that remains more or less constant; it is also called the constant-speed CME. On the other hand, the slow CME starts with a low initial speed, but shows a gradual acceleration; it is also called the accelerated and slow CME. Low and Zhang [Astrophys. J. 564, L53–L56, 2002] suggested that these two classes of CMEs could be a result of a difference in the initial topology of the magnetic fields associated with the underlying quiescent prominences. A normal prominence magnetic field topology will lead to a fast CME, while an inverse quiescent prominence results in a slow CME, because of the nature of the magnetic reconnection processes. In a recent study given by Wu et al. [Solar Phys. 225, 157–175, 2004], it was shown that an inverse quiescent prominence magnetic topology also could produce a fast CME. In this study, we perform a numerical MHD simulation for CMEs occurring in both normal and inverse quiescent prominence magnetic topology. This study demonstrates three major physical processes responsible for destabilization of these two types of prominence magnetic field topologies that can launch CMEs. These three initiation processes are identical to those used by Wu et al. [Solar Phys. 225, 157–175, 2004]. The simulations show that both fast and slow CMEs can be initiated from these two different types of magnetic topologies. However, the normal quiescent prominence magnetic topology does show the possibility for launching a reconnection island (or secondary O-line) that might be thought of as a “CME’’.     

机翼低雷诺数流动的数值模拟

通过SIMPLE方法求解非定常不可压N-S方程,研究了小展弦比机翼在低雷诺数下的流场特征,并分析其对气动特性的影响。研究对象为展弦比为1.0的平板矩形翼,进行了不同攻角的数值模拟,模拟雷诺数为1×105。分析表明:在小攻角时,主涡不断的从机翼上表面脱落;在大攻角时,受翼尖涡的影响,分离涡保持在机翼的背风面不脱落,形成驻涡。通过对流场分析,低雷诺数前缘层流分离和翼尖涡对小展弦比机翼的空气动力学特性起了决定性作用;使低雷诺数小展弦比矩形翼出现非定常、非对称和驻涡等现象。     

SMA 智能复合构件控制裂纹的数值与试验研究

将ＴｉＮｉ形状记忆合金（ＳＭＡ）薄带复合于基体材料内部,利用形状记忆合金的特性,可以控制构件裂纹的扩展。本文介绍了智能复合构件控制裂纹的机理,并利用拟温度载荷法,直接应用现有有限元程序对控制裂纹的ＳＭＡ智能复合构件进行了计算与分析,同时还进行了激光云纹干涉法试验测试。计算和试验结果表明智能复合构件中的记忆合金薄带对构件裂纹有显著的控制效果,同时计算和试验结果的一致性也表明本文的分析方法是可行的。     

B／Al单向铺层复合板的力学性能及断裂行为的研究

研究了热压扩散结合工艺对Ｂ／Ａｌ复合材料的强度的影响,并对试样拉伸断口及断裂径进行了研究,分析表明,试样断口有三种断裂模型,断裂路径同热压工艺有密切的关系。     

两种中温固化胶粘剂的剪切疲劳和蠕变性能研究

研究了SY 2 4B胶膜和SY H2糊状胶粘剂的剪切疲劳和蠕变性能。SY 2 4B胶膜和SY H2糊状胶粘剂同为中温固化的结构胶粘剂 ,SY 2 4B胶膜采用橡胶增韧 ,SY H2糊状胶粘剂采用热塑性树脂增韧。SY 2 4B胶膜虽然具有优异的韧性 ,但SY H2糊状胶粘剂的剪切疲劳和蠕变性能优于SY 2 4B胶膜 ,这与增韧剂种类与胶层厚度有一定关系。温度、应力和时间也是影响蠕变量的重要因素     

双定子涡流制动器电磁参数对制动力矩的影响

介绍了双定子涡流制动器(DSECB)的工作原理。根据等效磁路法推导了DSECB制动力矩公式。利用有限元法对DSECB进行了3D仿真分析。详细分析了DSECB各电磁参数对制动力矩特性曲线的影响,为DSECB优化设计提供了参考依据。     

A Class of TVD Type Combined Numerical Scheme for MHD Equations With a Survey About Numerical Methods in Solar Wind Simulations

It has been believed that three-dimensional, numerical, magnetohydrodynamic (MHD) modelling must play a crucial role in a seamless forecasting system. This system refers to space weather originating on the sun; propagation of disturbances through the solar wind and interplanetary magnetic field (IMF), and thence, transmission into the magnetosphere, ionosphere, and thermosphere. This role comes as no surprise to numerical modelers that participate in the numerical modelling of atmospheric environments as well as the meteorological conditions at Earth. Space scientists have paid great attention to operational numerical space weather prediction models. To this purpose practical progress has been made in the past years. Here first is reviewed the progress of the numerical methods in solar wind modelling. Then, based on our discussion, a new numerical scheme of total variation diminishing (TVD) type for magnetohydrodynamic equations in spherical coordinates is proposed by taking into account convergence, stability and resolution. This new MHD model is established by solving the fluid equations of MHD system with a modified Lax-Friedrichs scheme and the magnetic induction equations with MacCormack II scheme for the purpose of developing a combined scheme of quick convergence as well as of TVD property. To verify the validation of the scheme, the propagation of one-dimensional MHD fast and slow shock problem is discussed with the numerical results conforming to the existing results obtained by the piece-wise parabolic method (PPM). Finally, some conclusions are made. This revised version was published online in August 2006 with corrections to the Cover Date.