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.     

两种轴线相交度测量方法的比较

介绍了两种用准直望远镜测量三轴转台轴线相交度的测量原理和实现方法,对两种方法进行了比较,并指出了测量中应注意的问题。     

三轴相交度的一种测量方法

介绍了三个回转轴相交度的一种测量方法，并进行了测量不确定度分析。     

N5A飞机失速警告器的安装与校准

探讨失速警告器的选位安装与校准问题。失速警告器的选位安装与校准均由试飞实验确定。提出了如何调整失速警告器安装位置和安装角的指导性原则,论述了用表速计量失速预警速度的理由。     

基于回转体CAD/CAPP结构的图形文件OpenGL处理技术研究

在计算机辅助车削加工自动编程系统中,利用CAD软件系统输入图形,并通过应用程序对其文件格式进行转化,变成CAPP模块所需的基于特征的数据结构。     

旋转同心双轴间流动的热态实验

某型发动机高、低压涡轮轴间环形气流通内的流动可以简化为两个独立旋转同心双轴环道内的流动问题。对其控制方程以及边界条件进行无量纲化，得出了实验准则，设计并建立了实验台，以实验方法研究了具有轴向通流的独立旋转同心双轴环道内的流动规律。结果表明，随着冷气雷诺数增大，阻力系数总体趋势减小；冷气雷诺数的影响远大于内轴和外轴旋转对流动的影响。     

发动机高速动平衡的振动相位分析

针对发动机转子高速动平衡转速波动、无法保证振动信号同步整周期采样的特点,提出了一种基于转速脉冲的振动信号重构技术,大大提高了相量测量的准确度和稳定性。经试验验证,这项技术是有效、可行的。     

磁制动对地壳板块运动影响的理论分析与实证研究

太阳和木星的自转是不均匀的，纬度愈高，自转愈慢。据此，作者推测液态外地核的自转，也存在类似的不均匀性，而这种不均匀自转将对地壳板块运动产生影响。利用磁流体力学理论，阐明这类星球自转的不均匀性，是磁制动的不均匀性引起的。研究了磁制动对地壳板块运动影响的途径及表现方式，并举出实例证明这些表现方式的确存在，从而证明磁制动是影响地壳板块运动的一个极为重要的因素。     

关于刚体转动的角速度和角加速度的讨论

在理论力学教学中，平面运动刚体的转动与基点无关的证明过于简单，本利用矢量代数的知识，证明平面运动刚体的角度与角加速度与基点的选择无关。     

太阳微波爆发频谱事件

国家天文台1.0-2.0GHz,2.6-3.8GHz太阳射电频谱仪从1994年1月和1996年9月投入观测至2000年4月10日记录到太阳射电爆发分别为297个和316个，取得了高质量的高时间分辨率，高频率分辨率的动态谱资料，为研究耀斑各种尺度的时间及空间演化过程提供了丰富的信息，1998年4月15日的共同事件在时间和频率上显示了丰富的幅度和结构的变化。