Unsolved problems of solar wind expansion: Can we learn anything from SOHO?

Some of the main problems of solar wind expansion are addressed. Emphasis is placed on solar wind acceleration and the mass flux problem. It is demonstrated how these two properties of the flow depend on other plasma parameters such as temperature, density and helium abundance. The importance of placing constraints on a given solar wind flow in the inner corona and at larger distances from the sun simultaneously, is also shown. Whether and how these constraints can be derived from observations carried out by SOHO instruments is then discussed.     

Low frequency turbulence and energy dissipation in the Solar Wind

The possibility to perform in-situ measurements of velocity, magnetic field, density and temperature fluctuations in the Solar Wind has greatly improved our knoweledge of MHD turbulence not only from the point of view of space physics but also from the more general point of view of plasma physics.These fluctuations on the one hand extend over a wide range of frequencies (about 5 decades), a fact which seems to be the signature of turbulent non-linear energy cascade, on the other hand display, mainly in the trailing edge of high speed streams, a number of striking features: (i) a high degree of correlation between magnetic and velocity field fluctuations, (ii) a very low level of fluctuations in mass density and magnetic field intensity, (iii) a considerable anisotropy revealed by minimum variance analysis of the magnetic field correlation tensor. More recently it has been stressed that MHD turbulence in the Solar Wind displays a clear intermittent character.The picture which emerges from the most recent analytical theories and numerical simulations is presented. In particular the observations which give us informations about the dissipation mechanism, which remains yet largely unknown, are discussed.     

风速垂直切变统计分析

由于观测资料垂直分辨率的限制和实际问题的不同需要，存在多种不同的风速垂直切变统计分析方案和差别较大的统计分析结果。文章给出微分切变、投影风速切变、气层平均切变、差分切变的定义；比较了当风随高度变化的函数不同时不同切变的差别；分析了气层厚度、测风平均时距、风速垂直插值方案等对风速垂直切变统计量的影响；最后给出中国及世界风速切变极值统计结果及估算。     

低速大尺寸传热风洞的研制

为进行航空发动机内特别是叶轮机械内的边界层、传热和气膜冷却研究，设计、建造了大尺寸低速回流式风洞。描述了风洞结构和设计中考虑的主要问题。风洞性能测试结果表明，试验段中的气流达到很高的均匀度，不用紊流发生器时可达到很低的紊流度，试验板上的边界层参数和换热系数都和公认的关系式符合良好。     

粘性对再入锥气动静稳定性的影响

本文研究粘性对四种再入锥：１０度尖锥、１１度小钝锥、小球头三锥体、大球头三锥体在零攻角附近的气动静稳定性的影响。     

舵模型风洞颤振试验中亚临界技术的应用研究

为降低模型和风洞设备的损坏率，用随机激励和频响函数分析法，测定进入颤振临界点之前舵面颤振试验模型在不同风洞气流动压下的模态频率和阻尼比，由阻尼外推法或稳定参数法确定颤振临界动压。数次进入颤振状态的试验结果证明，所获得的颤振临界参数有较高的精度。     

锤头体弹性振动跨音速气动阻尼系数的确定

通过研究锤头形运载火箭跨音速飞行时，箭体结构的弹性振动与气体运动的耦合效应，描述了用全弹模型的风洞实验和非定常数值计算、确定气动阻尼系数的技术和方法，分别给出了实验和数值模拟的结果，并对结果进行了对比分析。结果表明，在气动阻尼实验中，模拟低阶固有模态的前节点位置是非常重要的，该方法可以作为研究航天飞行器非定常飞动特性的一种方法。     

地效飞机空气动力特性测量

介绍地效飞机带螺旋桨动力模型的风洞试验结果，着重介绍地面效应和螺旋桨转速参数对飞机气动力特性的影响。测量结果表明，地面效应非常明显，飞机升力和纵向稳定性都有明显增加。螺旋桨转速增加，使飞机升力增加，阻力减小，从而使升阻比有较大增加，同时使飞机纵向稳定性稍有降低。     

An engineering model of Titan surface winds for Dragonfly landed operations

Winds near the ground on Titan for the Dragonfly landing site (near Selk crater, 10°N) for the mid-2030s (Titan late southern summer, L_s ~ 310°) are estimated for mission design purposes. Prevailing winds due to the global circulation are typically 0.5 m/s, and do not exceed 1 m/s. Local terrain-induced flows such as slope winds appear to be similarly capped at 1 m/s. At various landing sites and times, these two contributions will vectorially combine to yield steady winds (for part of a Titan day, Tsol) of up to 2.0 m/s, but typically less – the slope wind component will be small in the mid-morning. In early afternoon, as on Earth and Mars, solar-driven convection in the planetary boundary layer will cause wind fluctuations of the order of 0.1 m/s, varying with a typical timescale of ~1000 s. Occasionally this convection organizes into coherent ‘dust devil’ vortices: detectable vortices with speeds of 1 m/s are predicted about once per Titan day. We have introduced the convective velocity scale combined with the advection time of PBL cells as a metric to derive the frequency of occurrence of gusts associated with convective vortices (‘dust devils’). Maximum possible vortex winds on Titan of 2.8 m/s may be expected only once per 40 Tsols, and define the maximum wind (4.8 m/s at 10 m height) that Dragonfly must tolerate without damage. The applicability of different wind combinations, scaled to the height of relevant Dragonfly components above the ground (e.g. the maximum corresponds to 3.9 m/s at 1.3 m height) by a logarithmic wind profile, to Dragonfly design and operations are discussed.