Spiral patterns with straight arm segments

The phenomenon of 'rows', which are straight geometrical segments in the spiral arms of galaxies, is studied. The Whirlpool nebula, Messier 51 (NGC 5194) in Canes Venatici, is considered to be an example of a giant grand design galaxy. Optical photographs, H α , ultraviolet and far-ultraviolet images, CO, 21-cm and synchrotron emission maps, and a K _s-band mosaic of M51 are studied. With this observational material, multiple rows can be recognized in the spiral arms of the galaxy. The rows comprise a major part of the arms. The lengths of the rows increase almost linearly with distance from the centre. They intersect one another at an (average) angle ≈2π/3. A possible physical explanation of the phenomenon of rows is discussed on the basis of the assumption that the formation of straight arm segments might be due to the gas-dynamical effect of stability of flat shock fronts, and the tendency of a slightly curved shock front to become flat. A quantitative flattening criterion enables an explanation of the geometrical properties of the arm patterns found in M51 and also in M101. A brief list of spirals with rows is given.     

台风的定常运动和螺旋斑图

应用控制台风的大气运动方程组求得了台风的三维定常流场以及相应的气压场和温度场,其中的三维流场构成了物理空间的一个非线性自治动力系统。研究指出:根据台风运动的定常解,台风的下层中心是低气压且是正垂直涡度(气旋式涡度)和水平辐合,上层中心是高气压(反气旋式涡度)和水平辐散;根据台风自治动力系统所获得的两个鞍一焦点很好地说明了台风的螺旋斑图,下层空气螺旋向内,引起台风中心附近的上升运动,上层空气螺旋向外引起台风外围的下沉运动,这些都与实际台风结构相似,文中阐明,地球的旋转和大气粘性对台风的螺旋结构是至关重要的。     

动态观测在软土地基路堤填筑施工中的应用

为了确保软土地基上修筑高速公路路堤的安全稳定,采用砂井预压排水固结法对京珠高速公路广珠段进行处理,并对地基土的变形进行动态观测,通过观测结果的综合分析,确定了合理的控制标准以指导施工。     

印度植被净初级生产力的时空变异及其影响因素分析

本研究旨在探讨1983-2008 年间印度植被净初级生产力(NPP)的时空变化格局及其与温度降水的关系。基于遥感数据和GLOPEM-CEVSA模型估算区域植被NPP,利用分段线性回归,分析了过去26年印度植被NPP的时空格局与变化特征。结果表明：（1）过去26年间印度植被年均NPP为414.29 gC·m^-2·a^-1,森林、农田和草地的NPP平均值分别为1002.32、485.98和631.39 gC·m^-2·a^-1。（2）分段线性回归结果显示,1983-2008 年间,印度植被总平均NPP呈先上升后下降的趋势,趋势转折点在1996年。占印度面积比例最大的农田植被类型的平均NPP也呈先上升后下降的趋势,趋势转折点在1996年,与总平均NPP的趋势转折点一致。（3）在空间上,印度大部分地区,发生了趋势转折,趋势转折点集中在1991-2000年间,大部分地区NPP在趋势转折点前呈上升趋势,其后呈下降趋势,与区域平均NPP的变化趋势一致。（4）印度西北部干旱地区植被NPP与温度呈负相关,与降水呈正相关。喜马拉雅山南部森林NPP则与温度呈正相关。降雨量较大的印度南部地区NPP与降水呈负相关。     

The effects of vertical viscosity coefficients with different distribution characteristics on classical Ekman spiral structure

The classical Ekman theory tells us that the ocean surface current turns to the right(left) side of wind direction with 45° in the north(south) hemisphere,but the observation and research results show that the surface current deflexion angle is smaller than 45° in the Arctic and high latitude areas while larger than 45° in the low latitude areas.In order to explain these phenomena,a series of idealized numerical experiments are designed to investigate the influence of vertical viscosity coefficients with different vertical distribution characteristics on the classical and steady Ekman spiral structure.Results show that when the vertical viscosity coefficient decreases with water depth,the surface current deflexion angle is larger than 45°,whereas the angle is smaller than 45° when the vertical viscosity coefficient increases with water depth.So the different observed surface current deflexion angles in low latitude sea areas and the Arctic regions should be attributed to the different vertical distribution characteristics of vertical viscosity coefficients in the upper ocean.The flatness of the Ekman spiral is not equal to one and does not show regular behaviors for the numerical experiments with different distribution of vertical viscosity.However,the magnitudes and directions of volume transport of Ekman spirals are almost the same as the results of classical Ekman theory,i.e.,vertical viscosity coefficient distributions have no effect on the magnitudes and directions of volume transport.     

基于CT成像的GBR术中两种植骨材料变化的比较分析

目的：利用CT扫描提供的图像信息与数据,运用Simplant软件分析系统,对GBR术中植入的天博骨粉（Bio—Osten）与Bio—Oss骨粉材料在引导骨生长过程中的体积变化进行定量比较分析,探讨天博骨粉的成骨状况。方法：选取15例前牙即刻种植同时实施GBR术的患者,随机分为两组,其中天博骨粉组（实验组）7例,Bio—Oss骨粉组（对照组）8例。在完成牙种植体植入的同时,植入天博骨粉或Bio-Oss骨粉,分别于术后1周、3个月、6个月进行种植区螺旋CT扫描,利用CT扫描提供的图像信息,运用Simplant软件分析系统,分别对即刻种植的GBR术后1周、3个月、6个月的天博骨粉、Bio—Oss骨粉的体积进行测量,计算其术后3个月、6个月时相对术后1周时骨粉的吸收率,并运用SPSS16．0统计软件包进行统计分析。结果：术后1周天博组、Bio—Oss组植入骨粉的平均体积分别为：101．10mm^3±14．76mm^3、121．69mm^3±38．35mm^3,两者无统计学意义（P〉0．05）;术后3个月天博组、Bio—Oss组吸收率分别为：41．51％±5．87％、49．30％±5．78％,差异有统计学意义（P〈0．05）;术后6个月,两者吸收率分别为：58．02％±5．67％、70．26％±10．64％,差异有统计学意义（P〈0．05）。结论：在CT影像上,天博骨粉与Bio—Oss骨粉有着相似的引导成骨性和可吸收性;相比较而言,天博骨粉的吸收速率慢于Bio—Oss骨粉,或者可能是Bio—Oss骨粉引导新骨生长速度快于天博骨粉。     

Orbits supporting bars within bars

High-resolution observations of the inner regions of barred disc galaxies have revealed many asymmetrical, small-scale central features, some of which are best described as secondary bars. Because orbital time-scales in the galaxy centre are short, secondary bars are likely to be dynamically decoupled from the main kiloparsec-scale bars. Here we show that regular orbits exist in such doubly barred potentials, and that they can support the bars in their motion. We find orbits in which particles remain on loops : closed curves which return to their original positions after two bars have come back to the same relative orientation. Stars trapped around stable loops could form the building blocks for a long-lived, doubly barred galaxy. Using the loop representation, we can find which orbits support the bars in their motion, and the constraints on the sizes and shapes of self-consistent double bars. In particular, it appears that a long-lived secondary bar may exist only when an inner Lindblad resonance is present in the primary bar, and that it would not extend beyond this resonance.     

Metallicity in damped Lyman-α systems: evolution or bias?

Assuming that damped Lyman- α (DLA) systems are galactic discs, we calculate the corresponding evolution of metal abundances. We use detailed multizone models of galactic chemical evolution (reproducing successfully the observed properties of disc galaxies) and appropriate statistics (including geometrical probability factors) to calculate the average metallicity as a function of redshift. The results are compatible with available observations, provided that observational biases are taken into account , as suggested by Boissé et al. In particular, high column density and high-metallicity systems are not detected because the light of backround quasars is severely extinguished, while low column density and low-metallicity systems are not detectable through their absorption lines by current surveys. We show that these observational constraints lead to a 'no-evolution' picture for the DLA metallicity, which does not allow us to draw strong conclusions about the nature of those systems or about their role in 'cosmic chemical evolution'.     

Effects of clumping on the observed properties of dusty galaxies

We present Monte Carlo radiative-transfer simulations for spiral galaxies modelled as a stellar disc and a two-phase clumpy dust distribution. We divide the volume occupied by the dust into a three-dimensional grid and assign each cell a clump or smooth medium status. Cell dimension, clump dust mass and spatial distribution are derived from the observed properties of giant molecular clouds and molecular gas in the Galaxy. We produce models for several values of the optical depth and fraction of the interstellar medium residing in clumps. As a general result, clumpy models are less opaque than the corresponding homogeneous models. For the adopted parameters, the increase in the fraction of energy that escapes the disc is moderate, resulting in surface-brightness profiles that are less than one magnitude brighter than those of the homogeneous models. The effects of clumping are larger for edge-on views of the disc. This is in contrast with previous preliminary results for clumping in the literature. We show how differences arise from the different parametrization and clump distribution adopted. We also consider models in which a fraction of the stellar radiation is emitted within the clumps. In this case, galaxies are less transparent than in the case when only dust is clumped. The opacity can be even higher than in the homogeneous case, depending on the fraction of embedded stellar emission. We point out the implications of the results for the determination of the opacity and dust mass of spiral galaxies.