螺旋桨滑流对带后缘襟翼机翼气动特性影响的数值分析

采用动量理论结合有限体积法求解N-S方程的方法,进行了螺旋桨滑流对带后缘襟翼机翼气动特性干扰的数值模拟分析.螺旋桨模型简化为一个激励盘,即一个无厚度可穿透的圆盘,以给定的圆盘拉力载荷,即压强差来模拟螺旋桨滑流的效果.采用嵌套网格技术处理桨盘与机翼间复杂的几何关系.算例计算表明,该计算方法能够较好的模拟滑流对带后缘襟翼机翼气动特性的影响.     

带襟、副翼三维机翼粘性绕流计算

运用嵌套网格方法严格考虑机翼切口和副翼、襟翼端面几何形状生成了合理的计算网格 ,并应用雷诺平均 Navier-Stokes方程和 Johnson-King湍流模型计算了带副翼三维机翼和带双襟翼三维机翼的粘性绕流。计算实践表明 ,用该方法可以很好地预计压力分布和最大升力。     

Gurney襟翼增升效应数值模拟

飞机的增升系统是影响其起降性的重要因素,为了系统地研究Gurney襟翼增升效应,本文采用数值模拟方法与结构网格求解不可压缩的Navier-Stokes方程对NACA0012翼型和机翼进行了研究。通过改变Gurney襟翼的高度、弦向位置来研究其对翼型气动特性的影响,并将结果应用于矩形机翼,计算结果表明:在一定范围内,Gurney襟翼越高、越靠近后缘则增升效果越好,在三维机翼上也具有相似的效果。     

涡襟翼及其与前端襟翼组合的气动特性

应用测压、测力、七孔管测速和激光流态显示等方法对三种(等弦长、分段、台阶)型式涡襟冀进行了实验研究,并和基本翼(74°后掠三角翼)作比较。发现单纯改变涡襟翼的形式和参数能提高减阻效果,但不能改变小迎角下升力过小的现象。为此将机翼前端作成襟翼形式(前端襟翼)并配置后缘襟翼,研究了两种前端襟翼对涡襟翼的干扰,实验表明适当控制前端襟翼使分离涡不破裂,可使该布局同时具有减小阻力和增加升力的效果。     

二维襟翼吹气控制的数值模拟

合理设计机翼翼型、前缘缝翼和后缘襟翼是飞机增升设计的重要手段,本文主要研究二雏襟翼吹气对翼型升力的影响。吹气襟翼的工作原理是,当襟翼偏转角较大时,由于翼面上表面的气流分离,此时达不到附着流所预计的升力值,可以在襟翼上表面进行吹气控制,吹除后缘的涡流而增大升力,得到预计的升力曲线。本文以NACA23018翼型为基础研究对象,采用非结构网格,在襟翼向下偏转角度45度的情况下,进行襟翼上表面的吹气效应数值模拟与流动控制机理的研究,结果表明此情况下襟翼上表面的吹气控制达到了增加升力和抑制分离的目的。     

前后缘机动襟翼数值计算研究

通过对前缘机动襟翼、后缘机动襟翼以及前后缘襟翼配合使用的状态作计算分析和比较，研究了机动襟翼在高亚音速段对构型气动特性的改善作用，为大后掠角、小展弦比机翼加装机动襟翼的改进设计提供了数值计算依据。     

小展弦比机翼加装格尼襟翼的低雷诺数试验

通过风洞试验研究了在低雷诺数下加装格尼襟翼的小展弦比机翼气动特性,机翼展弦比为1.67,格尼襟翼为1%~4%弦长高度,试验雷诺数分别为2.0×105和5.0×105.天平测力和表面测压的试验结果表明:低雷诺数下小展弦比机翼加装一定高度的格尼襟翼后,升力系数明显提高,加装1%弦长高度的格尼襟翼还能够提高机翼的升阻比.这是因为在试验雷诺数下,合适高度的襟翼在提高了机翼升力的同时并未显著增大机翼阻力.对比不同试验雷诺数下格尼襟翼的作用效果,表明格尼襟翼能够减少低雷诺数气流分离的不利影响,并且在较小的雷诺数下这种作用更加显著.关于格尼襟翼对低雷诺数层流分离现象的影响,还需要通过细致的流场显示技术进行研究.      

用有限基本解计算喷气襟翼气动特性

本文介绍使用有限基本解方法对喷气襟翼作气动力分析计算的方法。在DJS-6计算机上对矩形机翼在不同攻角,不同喷气角和不同喷气动量系数情况下作了一系列计算,计算的结果表明,用有限基本解方法来计算喷气襟翼的气动特性是可取的。对二元矩形喷气襟翼的计算结果与国外的某些计算和实验结果作了比较,对三元矩形喷气襟翼的计算是本文对这一问题的一个新的尝试。     

涡桨飞机滑流影响的非定常数值模拟验证

通过求解绝对坐标系下的非定常雷诺平均Navier-Stokes方程,计算了螺旋桨非定常滑流对某涡桨飞机起飞构型低速状态的气动特性影响。为描述螺旋桨桨叶的相对运动,采用了动态重叠网格技术,并在并行环境下采用全隐式双时间步方法和多重网格技术来保证时间精度和提高计算效率,计算结果与试验值相当吻合,研究表明:滑流区内襟翼上的动压得到明显增强,同时高速滑流也起到一个吹除在大偏度襟翼上堆积的附面层作用,延迟了襟翼上气流的分离,这两个因素明显提高了襟翼效率,另外经过机翼的导流作用后,滑流对襟翼的洗流不像机翼那么明显。本文还将有无滑流的流场进行对比,通过当地动压增量来定义滑流的加速效应边界,以及通过当地气流角增量来定义滑流的洗流效应边界。该方法能较好地捕捉和解释滑流对飞机部件干扰而使得飞机方向安定性呈现的非线性现象,初步揭示了螺旋桨滑流复杂尾迹流动的特点。     

螺旋桨对襟翼增升效果影响的数值模拟

寻找增大起降升力系数、降低起降距离的方法,一直是飞机设计领域的重要研究问题。文中通过数值模拟的方法,研究了螺旋桨滑流对飞机机翼和襟翼气动特性的影响。计算结果表明,螺旋桨的滑流对襟翼的增升有显著的提升效果,并且随着襟翼的偏转角度增大及螺旋桨的转速的提高越大,该效果也会进一步增强。通过该研究,在飞机设计时可以综合考虑上述影响,选取合适的螺旋桨和襟翼进行配合,找到螺旋桨的最佳位置,得到最大的升力系数,降低起降场长。     

机身上翘后体绕流与阻力分析

基于N－S方程数值计算研究了九个机身上翘后体在零迎角、高亚音速时的绕流与其阻力之间的关系。结果表明，后体在零迎角时存在三种流型：随着流型、分离涡流型和底部分离流型；影响阻力最大的几何参数是后体收缩比，其次是上翘角；收缩比ηA较大时（如ηA≥0．5），会产生很大的底阻；上翘角增加则使压差阻力迅速增大。当收缩比ηA减小的（即尾部较尖）使底部分离引起的粘性压差阻力大大减小，从而可实现最小的后体阻力。因此，首先选择较小的ηA排除底部绕流分离流型的出现、再选择适中的上翘角是上翘后体设计的一项重要原则。     

超高速高焓流动研究进展

本文介绍了中国科学院高温气体动力学重点实验室在超高速高焓流动模拟技术和试验方法方面取得的研究进展.文章主要包括三部分研究内容:第一部分是关于发展先进的超高速试验模拟技术,包括爆轰驱动高焓激波风洞和爆轰驱动高焓膨胀管.高焓激波风洞产生的超高速气流速度的范围是3.5km/s～6.0km/s,高焓膨胀管能够模拟速度为6.5km/s～10km/s的超高速气流.第二部分介绍高焓激波风洞喷管流场诊断结果,用来检验喷管产生的超高速流场的流场品质及其与飞行条件的差异.第三部分是关于超高速流动的试验方法和数值技术研究,包括高焓流动中真实气体效应对飞行器俯仰力矩变化的影响;热化学反应流动中表面催化效应诱导的气动热变化规律;喷管流场的气流非平衡效应对试验结果可能产生的影响.     

导弹水下发射时喷管的气体流动

针对导弹水下发射时喷管的气体流动问题，建立了水下喷管流的简化模型，定性地研究水环境的惯性对水下喷管内气体流动造成的阻滞作用。计算显示受阻滞流量△Q及受阻滞时间△t和喷管的喉部面积At呈幂函数关系，固定其他参数仅改变水深，△Q及△t和进口处气体的滞止压力p0与当地水下静压之间的压力差也有幂函数关系。结果表明喷管所处的水下深度越大，喷管内气体流动受阻滞状况也就越严重，而减小喉部面积At和适当增加膨胀比Ab/At以及增加滞止压力po，均有助于改善水环境对喷管喷出气体造成的阻滞状况。     

On management and control of turbulent shear flows

Concepts of turbulent flow control have become of growing importance during the last few years, following increased interest in the detailed structural scenario of turbulence—in particular our improved understanding of coherent structures on the one hand (the prerequisite), and a need for improvement of technological processes on the other (the goal). These considerations have mainly been followed by engineers and physicists concerned with problems in aerodynamics. It is our aim to draw the attention of a wider group of engineers to turbulent flow control in order to speed up the transfer of knowledge from aerodynamics to applications in other fields of engineering.

In this paper an attempt is made to compile a major body of the available knowledge on flow control in separated and wall bounded turbulent flows. After a brief introduction of the basics of control theory (Section 2) and of the major flow structures and their stability characteristics (Section 3) free and wall bounded turbulent shear flows are discussed (Sections 4 and 5). This discussion summarizes the main relationships between structure and flow behaviour and shows possibilities of influencing properties of these flows such as increasing mixing or avoiding separation.     

抛物化Navier-Stokes方程在求解高超声速流动稳定性分析 的基本流中的应用

通过在边界层内部使用边界层上缘的流向压力梯度代替该处的流向压力梯度,对传统抛物化Navier-Stokes(PNS)方程求解中的流向压力梯度的处理方法进行改进,从而使它可以求解用于稳定性分析的高超声速流动的基本流,并分别计算了平板、零攻角钝锥和小攻角钝锥三种典型算例.对于流向没有分离,且横向流动不强的流动,使用PNS方程计算高超声速流动稳定性分析用的基本流是可靠的.特别是改进后的方法求得的基本流的稳定性分析结果与直接求解Navier-Stokes(N-S)方程的结果非常吻合,但计算的时间消耗和空间占用都减少了一个数量级.     

Investigation of the stability of inviscid compressible swirling flows

The stability of an inviscid compressible swirling flow between two concentric cylinders is analytically investigated. Two stability criteria are derived for compressible swirling flows under narrow gap approximation by an analytic method analogous to Ludwieg's method. Finally, the effect of compressibility is discussed.     

Fuel atomization and mixing in unsteady swirling flows behind the gas-dynamic stabilizer

Features of fuel atomization and propagation in the flow behind a gas-dynamic stabilizer are considered. Estimations of the influence of transverse jets impulse magnitude on characteristics of mixing behind the stabilizer are obtained by numerical and experimental methods.     

Models of coronal hole flows

Models of plasma flow in a coronal hole fall naturally into four classes. These are: (i) radial flow on a streamline along which the divergence is assumed to vary differently than as the square of the radial distance from the Sun; (ii) global flow along streamlines determined in some independent manner; (iii) empirical models originating in, or based strongly on observation; (iv) dynamic models using magnetic and plasma boundary conditions low in the corona to find both the geometry of streamlines and the flow field.To date, models both of ideal coronal holes and of specific observed coronal holes indicate that flow velocities above 100 km s⁺¹, and temperatures of perhaps 2 × 10⁶K are possible at 2R heliocentric distance, where densities of 2 × 10⁵ cm⁺³ have been reported. These velocities are at, or just above the sound speed, although still sub-Alfvénic. There is also general agreement among models of large polar holes that conversion of mechanical wave energy flux into solar wind kinetic energy is occurring in the 2R to 5R range, perhaps occurs even further outwards, and that the magnitude and extent of this energy deposition depends on the size and on the geometrical divergence of the hole.However, each model exhibits distinct weaknesses counteracted only by the complimentary nature of the various types of models. Models in class (i) are simply not global representations, but are tractable when dealing with complex forms of the energy equation or with several ion species. Class (ii) models lack any geometrical information beyond the ad hoc assumption of known streamline geometry, but have the same advantages as those in class (i). Class (iii) models cannot determine streamline geometry within a hole and do not extend further from the Sun than the available data — although they place important constraints on models in the other classes. Class (iv) models are limited to simple forms of the energy equation and/or to quasi-radial flow, but are the only models producing self-consistent streamline geometries through inclusion of transverse magnetic stresses in the momentum equation.Most limitations in coronal hole flow models can be eliminated by using known numerical techniques to combine models in classes (i), (ii), and (iv). This would allow detailed models of coronal holes and corresponding interplanetary conditions to be developed for specific time periods, at the cost of flexibility and possibly also general conceptual understanding. Nevertheless, the concept of a coronal hole is now reasonably well established, and acceptable modelling approaches are rapidly filling the literature. It can be anticipated that the evolution of these models, together with present and future observations, will bring us much nearer to understanding coronal energetics and dynamics.Proceedings of the Symposium on Solar Terrestrial Physics held in Innsbruck, May–June 1978.     

Simulation of pulsating channel flows

A method for simulating spatial-temporary characteristics of pulsating flows in the varying-in-length-area channels based on the solution of one-dimensional nonstationary equations of gas dynamics is presented. The calculation results are compared with the experimental data, and it is shown that the method being proposed rather adequately simulates real processes in complex unsteady flows.     

Mass flows in coronal loops

Although static loop models are often used to describe the structure of coronal loops, it is evident on both observational and theoretical grounds that mass motions play a crucial role in the physics of the corona and transition region. First we review the observations of emission-line broadening and wavelength shifts, which imply the presence of random motions and systematic downflows in coronal loops. Some discrepancies in the observations are discussed. It is argued that velocities due to gas pressure gradients are the most likely explanation for the observed flows. A number of models that have been proposed for these motions are reviewed. The implications of the various models on observations of the corona and transition region by SOHO are discussed.