螺旋CT三维重建在骨盆骨折中的应用

目的：探讨用螺旋CT三维重建评价骨盆骨折的临床应用价值。方法：收集骨盆骨折17例，采用螺旋CT三维重建检查。结果：17例检查均取得清晰立体图像，且可消除某一骨性结构，单独观察骨盆某一组成骨的骨折情况。结论：螺旋CT三维重建在骨盆骨折的诊断、手术方案的设计及教学等有较高价值。     

高压旋喷桩桩周土摩阻力的分析与探讨

通过对旋喷桩的单桩静载试验，探讨了桩周土摩阻力作用的情况，通过计算和分析，得出了两个结论，为旋喷桩基础的设计提供参考。     

福建龙永煤田二叠纪(竹蜓)生物带的面貌特征与对比

研究地层是有效寻找沉积矿产的重要基础,将龙永煤田内关于的层位及分带性与大区域上的相似层位作了对比,并论述了本煤田的特征与变迁的基本过程。最后,结合多年来的研究成果,就煤田内的产出情况,作了两点必要的说明。     

TGQ系列勘察取样钻机(具)的研究

取样钻技术是区域地质填图、物化探取样、古地磁取样、地质灾害预警防治和工程勘察等必不可少的技术手段。TGQ系列勘察取样钻机包括TGQ-1、5、10三个型号，分析了其结构、特性和特点，以及配套钻具和取样器。     

桂林市2005年6月连续性暴雨的季风扰动及动力条件分析

通过对2005年6月连续性暴雨过程发生前后的天气形势和物理量场进行分析,发现暴雨发生时,与500hPa螺旋度、涡度及850hPa水汽通量配置较好。暴雨前期低空急流加强,表现在暴雨发生前850hPa沿110°E有V分量的增长。另外,可通过对T 213物理量预报场的分析,判断未来暴雨发生的可能性。     

Essential properties of the cD galaxy in Abell 1795 — II. Radio structure

We consider current problems connected with the evolution of central dominant (cD) galaxies in clusters. In the second part of this series, internal properties of the cD galaxy — in particular its radio structure — are related to the appropriate ones of the cluster. The observations point to an earlier jet ejection along the major axis of the galaxy and a following change of the jet axis. From the existence of “hot-spot” like regions in different directions it is suggested that the radio engine would have to be intermittent with a relatively short period. Alternatively to the intermittent ejection scenario, the radio morphology of 4C 26.42 can be explained in the frame of the “standard” beam or jet model. The radio structure of 4C 26.42 being an inversion-symmetric configuration, which is probably due to galactic cannibalism, could be interpreted as a transition at the inner hot spots (at about 1 kpc) from supersonic, stable Fanaroff-Riley type II jets to subsonic, unstable FR I type structures (“plumes”). A quantitative investigation of the two scenarios for jet interaction with the surroudning interstellar/intercluster medium in 4C 26.42 gives parameter values in reasonable agreement with the ones discussed in the literature for related objects.     

On the total kinetic energy of our galaxy

The total kinetic energy of the Galaxy is estimated from the potential energy by applying the virial theorem. The limits of the potential energy depend strongly on the value of the local escape velocity. They are estimated to be between −7. 10¹⁶ M_Ȯ km²s⁻² and −1. 10¹⁶ M_Ȯ km²s⁻² (escape velocity approximately between 450 km s⁻¹ and 600 km s⁻¹). The specific kinetic energy of the Galaxy as a whole is most likely about 21 000 km²s⁻², being equally distributed among the subsystems if the local escape velocity is near its lower limit; the higher the local escape velocity is, the higher is the specific kinetic energy of the Galaxy due to the influence of the dark corona. The specific kinetic energy of the dark corona tends to become equal to that of the Galaxy as a whole for very high values of the local escape velocity. For the purpose of estimating the totl potential energy of the Galaxy, inter alia, a new model of the Milky Way is developed, which yields both the potential and the density analytically so that it is suitale for calculating the galactocentric orbits.     

Essential properties of the cD galaxy in Abell 1795 — I. General optical and X-ray structure,dynamics and formation

We investigate current problems connected with the formation of cD galaxies. The subject of the present paper is to compare internal properties of the cD galaxy Zw162010 with cluster properties of Abell 1795. This consideration is a first attempt to find commonly valid essential correlations between peculiarities of brightest cluster members as structures and active phenomena and global cluster properties as for instance galaxy populations and concentration degrees. The colours, the X-ray emission, and the velocity of the cD galaxy are used to discuss the obvious influence of the environment on the evolution of the active nucleus. In a second paper (Kirchner et al. 1992) the radio structure is used to investigate the influence of the surrounding cluster medium onto the development of the active nucleus. Furtheron, various jet ejection scenarios will be quantitatively examined.     

The irregular galaxy Cassiopeia 1 – a new member of the Local group

A photometry in the V, R, I (Cousins) system has been performed for stars in the galaxy Cassiopeia 1. The resulting colour-agnitude (CM) diagram of Cas 1 reveals the existence of blue stars and the absence of red ones. From an analysis of the CM diagram of the galaxy it is concluded that A_v = 4.0 mag, and the distance modulus (m – M)_o = 24.5 mag, corresponding to a distance of 790 kpc. The visual magnitude of the galaxy is V = 14^m.62 (M_v = −13^m.8) and the colour index (V – R) = 0.89 mag. From the distance determination the galaxy Cassiopeia 1 is a member of the Local group.     

Photometric catalogue of Shakhbazian compact groups of galaxies. IV.

The fourth part of the photometric catalogue of Shakhbazian compact groups of galaxies contains optical and geometrical properties of another 26 groups (Shkh 313, 314, 315, 316, 317, 318, 319, 320, 321, 322, 323, 324, 325, 326, 327, 328, 329, 330, 331, 332, 333, 334, 335, 336, 337, 357). As in the previous papers photometric data were obtained from the COSMOS/UKST catalogue of the Southern sky with δ ± +2°30'. The survey of compact galaxy groups by Shakhbazian, Petrosian, Baier, and Tiersch is a basis for studying physical properties of such groups.