数据库系统研制中的几个实用技术     

李桐林  赵海珍 《铀矿地质》2000,16(6):375-379

本文根据几个数据系统开发发的实践经验,针对距平台数据导入,无ＤＳＮ连接、动态结账,软、硬盘备份恢复,控件优化等方面提出了几种简洁有效的实用技术。  相似文献   

Horizontal vibrations of a disk on a poroelastic half-space     

Bo Jin  Hua Liu 《Soil Dynamics and Earthquake Engineering》2000,19(4)

This paper analytically examines the horizontal vibration of a rigid disk on a saturated poroelastic half-space. The pressure-solid displacement form of the harmonic equations of motion for asymmetric dynamic problem are developed from the form of the equations originally presented by Biot. Making use of a new method the solution of the above equations is obtained. According to the mixed boundary -value conditions, the dual integral equations of the horizontal vibration of a rigid disk on a saturated poroelastic half-space are established. By appropriate transforms, it is shown that the dual integral equations can be reduced to a pair of Fredholm integral equations of the second kind, whose solutions are then computed. Numerical results for the horizontal dynamic compliance coefficient are given at the end of this paper.  相似文献   

Energy release on the surface of a rapidly rotating neutron star during disk accretion: A thermodynamic approach     

N. R. Sibgatullin  R. A. Sunyaev 《Astronomy Letters》2000,26(12):772-778

The total energy E of a star as a function of its angular momentum J and mass M in the Newtonian theory, E=E(J, M) [in general relativity, the gravitational mass of a star as a function of its angular momentum J and rest mass m, M=M(J, m)], is used to determine the remaining parameters (angular velocity, chemical potential, etc.) in the case of rigid rotation. Expressions are derived for the energy release during accretion onto a cool (with constant entropy), rapidly rotating neutron star (NS) in the Newtonian theory and in general relativity. A separate analysis is performed for the cases where the NS equatorial radius is larger and smaller than the radius of the marginally stable orbit in the disk plane. An approximate formula is proposed for the NS equatorial radius for an arbitrary equation of state, which matches the exact equation of state at J=0.  相似文献   

Dynamical properties of a centrifugally driven outflow from a disc near a black hole     

Xinwu Cao 《Astrophysics and Space Science》1995,226(1):165-168

The inclination of the field lines at the surface of the disc plays a crucial role on the nature of the magnetically driven flows. For the non-relativistic case, a centrifugally driven outflow of matter from the disc is possible, if the poloidal component of the magnetic field makes an angle of less than a critical 60° with the disc surface (Blandford and Payne 1982). We investigate the dynamical properties of the magnetically driven flows from the disc near a non-rotating black hole and find that the critical angle becomes larger than 60° when the flows start from the region near the black hole.  相似文献   

修正的粘滞律及有磁吸积盘的稳定性研究     

吴少平  吴学兵 《天文学报》1995,36(3):252-260

本文采用修正的粘滞定律及磁流体力学研究了薄吸积盘内区及外区的稳定性问题。运用微扰方法导出了色散方程，分析了四种情况下吸积盘的不稳定性，结果表明：在同时考虑磁场和修正的粘滞律时，吸积盘中存在着三种振荡模式，其中粘滞模式总是稳定的，磁声速模式（包括向里、向外传播两种模式）通常是不稳定的。这些结果为解释ＢＬ Ｌａｃ天体、Ｓｅｙｆｅｒｔ星系、类星体等活动星系核的光变现象提供了理论依据。  相似文献   

A unified description of the global structure of accretion disks     

Xing-ming Chen  Xue-bing Wu  Yong-heng Zhao 《Chinese Astronomy and Astrophysics》1996,20(4):409-414

The global structure of accretion disks is investigated in a unified scheme. We use a general radiative cooling formula applicable to both optically thick and thin regimes and we include radial advection cooling. Within the -viscosity models, we found distinct families of global solutions. If the accretion rate is low, there are three non-intersecting solutions, corresponding to optically thick and thin, local cooling and optically thin advection cooling. If the accretion rate is high, and the viscosity coefficient is large, the two local cooling solutions coincide at radii R₁ and R₂ and exist independently below R₁ and above R₂ while the advection solution is stable at all radii. If the accretion is high and the viscosity is low, the two optically thin solutions will cross each other while the optically thick solution exists at all radii.  相似文献   

窄吸积环动力学不稳定性的数值解     

刘仁杰  王德育 《天文学报》1995,36(2):159-164

本文在细环近似和共转半么位移不为零的条件下，考虑吸积环中非轴对称动力学不稳定性的线性扰动过程，采用数值计算方法求得不稳定性的线性增长率和共转半径位移随波数的变化关系，发现线性增长率受共转半径不为零的影响较小，而共转半径位移项随波数的色散关系与线性Ｋｄｖ方程的色散关系相同，说明窄吸收环在动力学不稳定性数值模拟中出现的“行星状解”很可能是类似于Ｋｄｖ方程中的孤子解。  相似文献   

Observations of disks around protostellar sources with nobeyama millimeter array     

Nagayoshi Ohashi  Masahiko Hayashi 《Astrophysics and Space Science》1995,224(1-2):13-16

We present results from a survey observation of circumstellar disks around protostellar sources associated with the Taurus molecular cloud. Our result shows that the 98 GHz continuum emission tends to be weaker for embedded sources than for visible T Tauri stars, which is consistent with our previous interpretation of disk formation. Direct observations of the formation of a centrifugally supported viscous accretion disk around HL Tau is discussed.  相似文献   

吸积盘整体结构的统一描述     

陈兴明  吴学兵  赵永恒 《中国天文和天体物理学报》1996,(3)

在考虑径向对流和不同光学厚度的基础上，我们采用一般的辐射致冷假设；在统一的框架内考察了吸积盘的整体结构．对α模型，我们发现在不同的盘区存在不同的整体结构．在吸积率较低时，存在三种类型解：光学厚的局部辐射致冷解；光学薄的局部致冷解；光学薄的对流致冷解．这些解在盘内较大范围内都存在且互不交叉．但在吸积率较高和粘滞系数较大时，两种局部致冷解会相互交叉，而对流为主的解在所有盘区都稳定存在．另一方面，在吸积率较高和粘滞系数较小时，两种光学薄解会相互交叉，而光学厚和局部致冷为主的解在所有盘区都存在．  相似文献   

太阳系行星系统的形成和演化     

陈丰  李雄耀  王世杰 《矿物岩石地球化学通报》2010,29(1):67-73

本文评述了星云和星子假说、太阳星云的崩塌、星盘的形成和演化、颗粒生长、星子增生、类地行星和类木行星的形成、行星迁移,以及太阳和行星的演化。  相似文献