Progress in the Study of Galaxies: Structures,Collective Phenomena and Methods

The review contains the important achievements in dynamics of the galactic disks. Among them there are I. New structures discovered recently: • giant vortices (including giant anticyclone in the Solar vicinity); • slow bar; • inner oscillating structure within spiral arms similar that of enveloped soliton; • chaotic streamlines in the velocity field of the gaseous disk of a real galaxy. II. New collective phenomina discovered recently: • new overreflection instability initiating ‘mini-spiral’ in the innermost central parsec of Galaxy; • large-scale convection caused by nonlinear interaction of density wave with disk gas; • non-kolmogorovian spectrum of weak turbulence corresponding to the observed one in the • Solar vicinity. III. New methods worked out recently: • reconstruction of full three-dimensional vector field of gas velocity from the observed line-of- • sight velocity field; • observational test for verification of the wave-nature of the spiral arms; • observational test to distinguish two types of vertical motions: warp and z-motions in the • density wave; • derivation of correct system of two-dimensional dynamical equations from the initial three- • dimensional one. This revised version was published online in June 2006 with corrections to the Cover Date.     

Galactic effects of the cosmic-ray gas

On an astronomical scale cosmic rays must be considered a tenuous and extremely hot (relativistic) gas. The pressure of the cosmic-ray gas is comparable to the other gas and field pressures in interstellar space, so that the cosmic-ray pressure must be taken into account in treating the dynamical properties of the gaseous disk of the galaxy. This review begins with a survey of present knowledge of the cosmic-ray gas. Then the kinetic properties of the gas are developed, followed by an exposition of the dynamical effects of the cosmic-ray gas on a large-scale magnetic field embedded in a thermal gas. The propagation of low-frequency hydromagnetic waves is worked out in the fluid approximation.The dynamical properties of the gaseous disk of the galaxy are next considered. The equations for the equilibrium distribution in the direction perpendicular to the disk are worked out. It is shown that a self-consistent equilibrium can be constructed within the range of the observational estimates of the gas density, scale height, turbulent velocity, field strength, cosmic-ray pressure, and galactic gravitational acceleration. Perturbation calculations then show that the equilibrium is unstable, on scales of a few hundred pc and in times of the order 2 × 10⁷ years. The instability is driven about equally by the magnetic field and the cosmic-ray gas and dominates self-gravitation. Hence the instability dominates the dynamics of the interstellar gas and is the major effect in forming interstellar gas clouds. Star formation is the end result of condensation of the interstellar gas into clouds, indicating, then, that cosmic rays play a major role in initiating star formation in the galaxy.The cosmic rays are trapped in the unstable gaseous disk and escape from the disk only in so far as their pressure is able to inflate the magnetic field of the disk. The observed scale height of the galactic disk, the short life (10⁶ years) of cosmic-ray particles in the disk of the galaxy, and their observed quiescent state in the disk, indicate that the galactic magnetic field acts as a safety valve on the cosmic ray pressure P so that PB ²/8. We infer from the observed life and quiescence of the cosmic rays that the mean field strength in the disk of the galaxy is 3–5 × 10^–6 gauss.     

基于等效盘模型的滑流对涡桨飞机气动性能的影响

 推导了螺旋桨等效盘模型的相关气动计算公式,建立了考虑螺旋桨桨盘前后压差和滑流旋转速度以及变桨距、螺旋桨转速等因素的较通用的等效盘模型。将等效盘边界条件应用于NAPA软件进行了三维流场计算,分析了流场计算结果和流场特征;并采用某螺旋桨的试验数据对等效盘模型进行了检验,推力和扭矩的计算值与试验结果吻合较好,表明该等效盘模型能较为准确地模拟螺旋桨的推力、扭矩、压力变化和旋转速度变化,能在一定程度上替代真实螺旋桨的气动效应。然后应用该等效盘模型对某四发涡桨飞机的全机三维流场进行了数值模拟研究,分析了螺旋桨滑流对全机流场特征的影响,给出了滑流对全机升、阻力系数的影响量。计算结果表明,螺旋桨后形成的涡能改变下游的流场并使机翼表面流线偏转,螺旋桨滑流能明显改变机翼表面的压力分布,使全机升、阻力系数增大,且滑流强度越大,效果越明显。     

发动机防冰支板水滴撞击特性的数值研究

在对发动机防冰支板附近的流场进行计算的基础上,使用离散相模型在拉氏坐标下模拟了该流场中过冷水滴的运动轨迹,对发动机防冰支板的水滴撞击特性进行了研究.研究表明,水滴撞击极限、总收集系数和局部收集系数随飞行高度、来流速度及水滴直径的增加而增大.     

Magnetospheric Models and Trajectory Computations

The calculation of particle trajectories in the Earth's magnetic field has been a subject of interest since the time of Störmer. The fundamental problem is that the trajectory-tracing process involves using mathematical equations that have `no solution in closed form'. This difficulty has forced researchers to use the `brute force' technique of numerical integration of many individual trajectories to ascertain the behavior of trajectory families or groups. As the power of computers has improved over the decades, the numerical integration procedure has grown more tractable and while the problem is still formidable, thousands of trajectories can be computed without the expenditure of excessive resources. As particle trajectories are computed and the characteristics analyzed we can determine the cutoff rigidity of a specific location and viewing direction and direction and deduce the direction in space of various cosmic ray anisotropies. Unfortunately, cutoff rigidities are not simple parameters due to the chaotic behavior of the cosmic-ray trajectories in the cosmic ray penumbral region. As the computational problem becomes more manageable, there is still the issue of the accuracy of the magnetic field models. Over the decades, magnetic field models of increasing complexity have been developed and utilized. The accuracy of trajectory calculations employing contemporary magnetic field models is sufficient that cosmic ray experiments can be designed on the basis of trajectory calculations. However, the Earth's magnetosphere is dynamic and the most widely used magnetospheric models currently available are static. This means that the greatest uncertainly in the application of charged particle trajectories occurs at low energies.     

Impact of gravitation on gaseous pollutant source identification

 It is necessary to identify a gaseous pollutant source rapidly so that prompt actions can be taken, but this is one of the difficulties in the inverse problem areas. In this paper, an approach to identifying a sudden continuous emission pollutant source based on single sensor information is developed to locate a source in an enclosed space with a steady velocity field. Because the gravity has a very important influence on the gaseous pollutant transport and the source identification, its influence is analyzed theoretically and a conclusion is drawn that the velocity of fluid is a key factor to effectively help weaken the gravitational influence. Further studies for a given 2-D case by using the computational fluid dynamics (CFD) method show that when the velocity of inlet is less than one certain value, the influence of gravity on the pollutant transport is very significant, which will change the velocity field obviously. In order to quantitatively judge the practical applicability of identification approach, a synergy degree of the velocity fields before and after a source appearing is proposed as a condition for considering the influence of gravity. An experimental device simulating pollutant transmission was set up and some experiments were conducted to verify the practical application of the above studies in the actual gravitational environment. The results show that the proposed approach can successfully locate the sudden constant source when the experimental situations meet the identified conditions.     

Analysis of the buoyancy-induced heat transfer in a rotating cavity

In order to get a better knowledge of the heat transfer in compressor cavities of aero-engines, the simplified rotating cavity with two-plane discs, a shaft and a cylindrical rim has been investigated numerically and compared with the available measurements. The numerical results in agreement with the available experiments show large-scale instabilities. The disk local Nusselt numbers show mainly radial rising distributions for the heated disks with radial rising temperature profiles. In the present work, at the Reynolds number of 20000, the disk local Nusselt numbers are the correlations of the local Grashof number to the power of 1.89~2.6, and the value of the power is increased as the rotational Reynolds number goes up. At the rotational Reynolds number of 800000, the local Nusselt numbers are the correlations of the local Grashof number to the power of 0.68~2.6, and the value of the power is decreased as Reynolds number goes up. The area-averaged disk Nusselt number is the correlation of the Reynolds number to the power of 0.479 and the rotational Grashof number to the power of 0.12.      

叉排型扰流柱排内部流场的实验研究

在特别建造的小型扰流柱排风洞上，测量了6个不同雷诺数下叉排型短扰流柱排内部的流场分布，发现不同雷诺数下流场分布非常相似，在奇数和偶数测量截面上，速度分布规律不同，在奇数截面上可以观察到通道涡，在偶数截面的端壁附近存在马蹄涡。     

基于CFD-DEM耦合数值模拟的全尺寸直升机沙盲形成机理

为了研究直升机发生沙盲时沙尘云在悬停流场中的状态和分布规律，采用基于雷诺平均Navier-Stokes方程和Menter 剪切应力输运（SST）k-ω湍流模型的数值模型，通过应用程序编程接口耦合基于Hertz-Mindlin （No Slip）碰撞接触模型的离散元模型，并基于"多球法"构建了更加真实的非球形沙尘颗粒，计算了沙尘颗粒在流场中的运动和分布状态。与可得到的试验结果进行对比，验证了数值方法的有效性，并进行了地效状态旋翼拉力系数、桨尖涡位置以及沙尘云形成的宏观轮廓图的计算。应用所建立的方法，对不同悬停高度的直升机地效流场进行了计算，给出了流场的涡量以及速度云图，着重对比了不同悬停高度下沙尘云中沙尘颗粒速度和分布情况，分析了地效流场对沙尘颗粒状态的影响及沙尘云的形成机理，并计算出了沙尘云宏观分布图。结果表明：流场中大部分沙尘颗粒只能在地表随流场扩散而并不能形成沙尘云；沙尘云中外层空间的沙尘浓度比内层高；位于桨盘平面下层区域的沙尘颗粒以径向运动为主，切向速度较小，而位于桨盘平面上层的沙尘颗粒速度方向各异，速度大小接近。     

Galaxien vom Magellanschen Typ

In the first part of this paper the morphological structure of Magellanic type galaxies (Irr I) is investigated. The galaxies of Magellanic type present a basic pattern consisting of a disk, a bar, stellar arms, rudimentary or well developed, spiral filaments and condensations in the disk. With the help of this pattern a well-defined classification scheme is set up. The subgroup of Irr II-systems consists of normal galaxies which are more or less tidally disturbed. Bursts of star formation have a great influence on structure and colour of irregular galaxies. Using the ESO-B Atlas, 580 galaxies of Magellanic type (out of a sample of 3187 galaxies) were classified; 57 are new SB(s)m systems (prototype Large Magellanic Cloud). The sample shows dominant bar structures at the classification stages d-, dm-, and m. A striking feature is the asymmetric position of bar and disk. This asymmetry is a general characteristic of galaxies of types SBd-SBm IB. The asymmetry can be discribed by a relative displacement parameter \(\tilde \Lambda \) = 0.78 ±0.15, defined as the quotient of small and great distance of the bar center to the optical edge of the disk. The displacement cannot be explained by tidal interaction with neighbouring galaxies. In the second part of the paper the kinematics and dynamics of the Large Magellanic Cloud (LMC) as the nearest and best-known example of a galaxy of Magellanic type is investigated. The main structural features of the LMC are disk, bar, rudimentary and well developed stellar arms as well as spiral filaments (not necessarily connected with density waves); the γ-structure is a broken up ring structure. Embedded into these features are young, asymmetrically located spiral arm filaments. As an explanation for these structures stochastic start formation in an ordered chain reaction is proposed. The pattern of the spiral arm filaments is determined by the rotation curve. The morphological peculiarities of the LMC can also be detected in other galaxies of that type. The mean absolute displacement of the centers of bar and disk, determined from 18 galaxies, is Λ = 800 pc. The displacement between the bar center and the symmetry center of the rotation curve is of the same order. The presently known radial velocities of planetary nebulae, star clusters, Hi and Hii regions and stars belonging to the LMC have been collected in a catalogue as the basis of a discussion of the kinematics and dynamics of the LMC. Contrary to earlier work, we have used, for the first time, the radial velocities of objects of all subgroups together by a proper weighting scheme. Thus the basic kinematics and dynamics of the LMC has been deduced. The radial velocity field shows no central symmetry; it is characterized by large scale (2–3 kpc) disturbances. By comparison with the velocity field of other galaxies three main disturbances are identified: an oval distortion of the velocity field in the bar region, a radial velocity field around 30 Doradus, and disturbances connected with a warp or material above the disk in the southern quadrants. The results of a detailed numerical analysis of these three facts can be summed up as follows:

1. The rotation curve is determined over 10° diameter; it shows differential rotation, an asymmetric behavior in the south and a double structure in its Hi component. The rotation center is displaced by 0°.7 from the bar center. The orientation of the kinematic line of nodes and the systemic velocity vary as functions of the distance from the center. Therefore, it is possible to show definitely that large scale disturbances (warping, z-structure and streaming motions) are existent.
2. By variation of the kinematical parameters (systemic velocity, inclination, orientation of the line of nodes, rotation center) the dispersion of the measured radial velocities was minimized and the basic rotation curve determined. The rotation curves for the north and south side of the LMC are significantly different. The south side is either warped or there is material above the main plane. There seems to be a connection between this structure, the Panmagellanic Gas and the Magellanic Stream. The north side appears to be free of distorsion.
3. The residual velocity field (observed minus model) deduced from a basic rotation curve shows that the displacement between the rotation center and the bar center is not caused by local streaming motions. The rotation center must be the mass center. The bar shows a radial velocity field; in the 30 Doradus region inward and outward motions are found.

The mean velocity dispersion of population I objects is 10.5 km s^-1 of population II objects 16.0 km s^-1. Red and blue globular clusters show different kinematical behavior. By comparison of eight mass models, taking into consideration thickness effects and controlled by surface photometric data, the mass of the LMC is found to be (0.5 ± 0.1) × 10¹⁰ \(\mathfrak{M}_ \odot \) (assuming the inclination 33°, the systemic velocity 46.9 km s^-1, and the distance 56 kpc). Dynamically, the LMC can be described by a dominating disk potential with an additional bar potential as a disturbance. The mass of the bar is 0.6 × 10⁹ \(\mathfrak{M}_ \odot \) . The stable neutral point of such a configuration can be found in the residual velocity field. The absorption feature crossing the bar coincides with the maximum velocity gradient of the computed radial velocity field in the plane of the system.     

速度比对气-气喷嘴燃烧性能的影响

为研究应用于全流量补燃循环发动机的气-气喷嘴,开展气氢/气氧为推进剂的同轴剪切喷嘴的热试试验研究。通过测量燃烧室压力和燃烧室壁面温度,研究氢氧速度比变化对燃烧效率和对燃烧室热载荷的影响。结果显示燃烧效率受到速度比和推进剂喷射绝对速度的影响;燃烧室热载荷随速度比增大而增大。气-气喷注器的设计应选择小的氧喷注压降和适合的速度比。     

螺旋桨旋转速度对机翼气动力影响的数值模拟

为了研究螺旋桨滑流中的旋转速度对机翼气动力的影响,分别采用非定常方法和桨盘理论两种方式对螺旋桨/机翼构型进行模拟。与非定常方法对比,桨盘理论足以模拟螺旋桨滑流对机翼的影响,并能降低计算要求,缩短计算时间。因此,采用桨盘理论研究桨盘扭矩载荷对应的旋转速度增量对机翼气动力的影响。计算结果表明,桨盘旋转速度对机翼升力影响不大,但是对零攻角时的机翼阻力存在特殊的影响。发现了这一影响,并对其原因进行了说明。     

Non-adiabatic Ion Acceleration in the Earth Magnetotail and Its Various Manifestations in the Plasma Sheet Boundary Layer

Many physical phenomena in space involve energy dissipation which generally leads to charged particle acceleration, often up to very high energies. In the Earth magnetosphere energy accumulation and release occur in the magnetotail, namely in its Current Sheet (CS). The kinetic analysis of non-adiabatic ion trajectories in the CS region with finite but positive normal component of the magnetic field demonstrated that this region is essentially non-uniform in terms of scattering characteristics of ion orbits and contains spatially localized, well-separated sites of enhanced and reduced chaotization. The latter represent sources from which accelerated and energy-collimated ions are ejected into Plasma Sheet Boundary Layer (PSBL) and stream towards the Earth. Numerical simulations performed as part of a Large-Scale Kinetic Model have shown the multiplet ion structure of the PSBL is formed by a set of ion beams (beamlets) localized both in physical and velocity space. This structure of the PSBL is quite different from the one produced by CS acceleration near a magnetic reconnection region in which more energetic ion beams are generated with a broad range of parallel velocities. Multi-point Cluster observations in the magnetotail PSBL not only showed that non-adiabatic ion acceleration occurs on closed magnetic field lines with at least two CS sources operating simultaneously, but also allowed an estimation of their spatial and temporal characteristics. In this paper we discuss and compare the PSBL manifestations of both mechanisms of CS particle acceleration: one based on the peculiar properties of non-adiabatic ion trajectories which operates on closed magnetic field lines and the other representing the well-explored mechanism of particle acceleration during the course of magnetic reconnection. We show that these two mechanisms supplement each other and the first operates mostly during quiescent magnetotail periods.     

水滴撞击特性的数值计算方法研究

 对水滴撞击特性的数值计算方法进行了研究。在对防冰部件流场进行计算的基础上,通过对水滴所在单元的判断和单元内流场速度的插值求解以及水滴运动轨迹计算边界的判断,采用差分法对水滴运动方程进行了数值求解,得到了水滴运动轨迹,从而确定了水滴的撞击极限、总收集系数和局部水收集系数等水滴撞击特性参数,为飞机防冰系统的设计奠定了基础;此外,以发动机进气道的水滴撞击特性的计算为算例,研究了飞行高度、飞行速度及水滴半径对水滴撞击特性的影响。     

The anchoring of gaseous jet diffusion flames in stagnant air

A numerical analysis is presented to describe the structure of the attachment region of gaseous jet diffusion flames in stagnant air. For the typical Reynolds numbers encountered in applications, the region of flame attachment, in the near wake at the injector rim, is small compared with the injector radius. The local flow, which we consider to be laminar, quasi-steady and two-dimensional, is determined by the wall value of the fuel stream velocity gradient and the chemical reaction time or residence time in the premixed flame of a stoichiometric mixture of the fuel stream and required amount of air. When the Karlovitz number, or product of the velocity gradient and the flame residence time, grows above a critical value the flame is lifted off the injector.     

环形燃烧室两相燃烧数值研究

根据环形燃烧室设计需要,运用计算机模拟技术研究模型环形燃烧室三维有旋液雾燃烧流场,研究两相流动与混合,液雾蒸发对燃烧过程的影响。两相流动模型采用颗粒群轨道模型,气相紊流输运方程求解采用双方程k-ε模型和EBU-Arrhenius紊流燃烧模型,热辐射采用热通量法模型,本文提供计算方法可以用来研究不同性能参数对环形燃烧室两相燃烧特性影响。     

Estimating the High-Resolution Mean Sea-Surface Velocity Field by Combined Use of Altimeter and Drifter Data for Geoid Model Improvement

The mean sea-surface height obtained from satellite altimeters is different from the geoid by the amount of mean sea-surface dynamic topography associated with ocean currents. Assuming geostrophy at the sea surface, the mean sea-surface dynamic topography can be obtained from the mean sea-surface velocity field. This field is derived by combining anomalies (i.e., deviations from the mean) of sea-surface velocity obtained from altimeter data and in situ surface velocities estimated from trajectories of surface drifting-buoys (hereafter, drifters). Where a drifter measured the surface velocity, the temporal mean velocity can be estimated by subtracting the altimeter-derived velocity anomaly at that time from the drifter-measured surface velocity. The method is applied to the surface flow field of the North Pacific, using TOPEX/POSEIDON and ERS-1/2 altimeter data, and WOCE-TOGA surface drifter data obtained from October 1992 through December 2000. The temporal mean velocity field is estimated with a resolution of quarter degrees in both latitude and longitude. The obtained mean velocity field clearly shows the Kuroshio and Kuroshio Extension, which are narrower and stronger than the climatological mean features derived from historical hydrographic data averaged over several decades. Instantaneous velocities are estimated by summing up these temporal mean velocities and anomalies, every ten days during the eight years. They compare well with in situ velocities measured by the surface drifters. The instantaneous velocity field shows energetic fluctuation of the Kuroshio Extension vividly. This revised version was published online in August 2006 with corrections to the Cover Date.     

双级轴向旋流器气量分配对流场特性影响的数值模拟与试验验证

为了探究双级轴向旋流器气量分配对流场特性的影响,对相同进口条件下不同旋流器流场特性进行数值模拟,并结合流量特性试验和粒子图像测速仪流场试验进行验证。结果表明:当第1、2级旋流器气量比由0.32增大到1.48时,旋流器下游轴向、径向速度降低,气流扩张角、回流区宽度以及回流率均减小;不同气量分配的第1、2级旋流在文氏管出口与套筒出口之间剧烈掺混,经过套筒出口后,旋流数均小于0.4;在相同的结构形式下,不同气量分配的双级旋流器通过改变第1、2级旋流器在文氏管出口处的旋流数,进而改变了第1、2级旋流相互掺混的强度,并最终影响了下游流场。     

航天器太阳圆面速度差/太阳视方向组合导航

针对航天器，尤其是深空探测器的自主导航问题，提出了一种新的太阳圆面速度差天文量测信息，该信息利用太阳的较差自转所造成的太阳圆面各点速度不同的特性，是探测器当前位置的函数，其几何本质是一个探测器的位置圆锥。在此基础上，基于太阳圆面速度差和太阳视方向互补的特性，提出了一种太阳圆面速度差/太阳视方向组合导航新方法，将太阳圆面速度差与太阳视方向2种量测量结合起来，实现了量测量之间的优势互补，进一步提高了导航性能。以太阳探测器为例进行了仿真，仿真结果表明相比较于单独用太阳圆面速度差或太阳视方向的导航方法，基于太阳圆面速度差/太阳视方向的组合导航方法精度分别提升了10.2%和16.0%。此外，还分析了光谱仪精度、采样周期和光谱仪数量对导航性能的影响，为深空探测自主导航提供了新的理论与方法。