基于有限单元热网络法的航空发动机主轴轴承热分析

航空发动机主轴轴承温度场的精准预测对保证发动机润滑系统及整机稳定运转至关重要。针对传统热网络法精度低的问题,提出一种基于有限单元思想的有限单元热网络法。将轴承结构通过网格划分为有限个单元体,每个单元体设置一个温度节点代表该单元体的集总参数,节点间构建热阻关系并形成热网络,通过求解以温度为未知量的大型稀疏矩阵线性方程组来获得滚子轴承横截面的温度分布。该方法可以与轴承局部产热理论相结合,实现轴承局部产热的精准加载,完成温度场的精细化分析。通过与试验结果对比,本文方法对轴承外环表面中心线温度的预测结果与试验结果误差不超过13%。     

基于多节点热网络法的航空发动机主轴轴承温度场分析

航空发动机主轴轴承温度场分析是发动机润滑系统热分析的关键。针对传统简单节点热网络法中轴承温度节点设置过于简化、人为设置轴承生热分配比例等问题,提出改进的多节点热网络法。基于Hertz热扩散理论,将轴承三元件分别划分为接触表面与主体两个节点,并以Hertz扩散热阻连接;轴承接触区设置油膜节点,加载轴承生热载荷,节点与轴承接触面之间通过油膜热阻连接;构建多节点轴承热网络模型,获得轴承内部更细致的温度场分布。研究表明,轴承表面温度显著高于其内部主体结构温度,而接触区对应的两个接触面之间也存在明显的温度差异,使用本文建立的多节点热网络法对滑油出口温度的计算误差不超过7%。     

基于PCA-TN的直升机主减速器通用热分析计算

针对当前热分析方法无法满足直升机主减速器结构复杂多变的问题,提出了一种快速获取主减速器温度场分布的通用热分析方法。以典型直升机主减速器为样本,进行了主成分分析（principal component analysis,PCA）,并结合热网络法（thermal network,TN）,分析获得3种通用热分析单元体模型。对于不同结构的主减速器,通过单元体及其衍生体的组合可以迅速且有效地建立其系统热分析模型,求解获得温度场分布。以某直升机主减速器为例,应用该方法进行了热分析,并与试验进行了对比,结果表明:该方法能高效计算主减速器的温度场分布,计算值与试验值最大误差为5.07%,满足主减速器热分析工程计算需求。      

某直升机齿轮传动系统的瞬态热分析

提出了传动系统瞬态温度场的分析方法,建立了失去润滑条件下传动系统功率损失及对流换热系数的计算模型,该模型考虑了失去润滑后传动系统热状态参数的时变特征。在稳态热分析的基础上,求解了某直升机齿轮传动系统的瞬态温度场,为该传动系统生存能力的预测提供了理论依据。      

飞机整体瞬态热状况的数值仿真研究

 在分析飞机内外热环境的耦合传热机制基础上，建立了描述飞机整体瞬态热状况的物理数学模型。引入壁面热流函数，将飞机蒙皮外的气动对流与辐射换热作用转化为舱内热分析的浮动热边界条件，实现了飞机内外耦合热作用的解耦计算，避免了难以实现的直接耦合求解。采用区域分解技术，将飞机整体分解为特性不同的多个求解区域。采用蒙特卡罗法求解舱内设备之间的辐射换热，采用热网络法求解设备内部及各设备之间的辐射-导热-对流耦合换热。利用该方法对某型飞机飞行过程中的瞬态热状况进行了数值模拟，获得了飞机舱内的瞬态温度场，分析了相关因素的影响，为飞机设计及相关研究提供了重要依据。     

航空发动机轴承腔热状态分析模型及温度场计算

分析了轴承腔的主要热源。建立了轴承及石墨密封摩擦热的计算模型、密封热泄漏量的计算模型、对流换热系数的计算模型及温度场的计算模型。用热网络法建立了轴承腔的热平衡方程组,并采用拟牛顿法求解了该方程组。获得了10种不同工况下的温度场计算结果,该结果与本文的测试结果基本吻合。      

单腔内冷涡轮的气热耦合数值仿真

将所开发的HIT-3D气热耦合求解器应用于某低压涡轮的数值仿真中,对该涡轮设计简单的内冷结构,比较了不同湍流、转捩模型对叶片温度场预测的影响,初步验证了所开发的耦合求解器的应用能力.由于目前涡轮的冷却结构复杂,数值计算量比较大,为此发展了一种气热耦合与工程设计相结合的方法,以该涡轮为算例初步验证了该方法,并初步模拟了粗...     

喷管温度场计算的加权余数有限元方法

喷管温度场计算是固体火箭发动机喷管设计中遇到的一个重要问题。利用差分法计算温度场已有很多文献报导,本文提供一个加权余数有限元法计算喷管的温度场,其突出的优点是能与热结构计算程序联用,组成热分析和热结构的统一程序,因为加权余数有限元与变分原理有限元在节点网格的划分,有限元几何参数的计算,变带宽的一维储存和代数方程组的求解都有相同之处。为了说明方法的精度和可靠性,本文给出了有限元计算与解析解的比较,有限元计算与地面试验结果的比较,这些比较表明:本文提供的方法是可靠的,可供     

石英挠性加速度计组件精密温控系统热分析

在捷联惯性导航系统中石英挠性加速度计是其核心器件,加速度计的温度 特性直接影响其测量精度。在高精度的惯性系统中,需要对加速度计组件进行精度优于 0.05℃的温度控制。为了研究加速度计组件精密温控系统,利用有限元分析软件ANSYS 建立石英挠性加速度计组件温控系统的有限元模型,仿真计算其有限元模型的温度场。 首先根据组件的结构特性建立了其有限元模型,介绍了热分析中求解条件的确定方法。 通过仿真得到温控系统的温度场模型,根据温度场模型计算温度梯度并且确定系统的测 温点、控制方式,最后利用加速度计输出数据验证分析结果的正确性。研究结果可以为 加速度计组件精密温度控制系统中的测温点选取、控制方式确定以及捷联惯导系统中温 度补偿、温度控制与热优化提供参考依据。     

飞行器热天线热电联合计算方法

为了研究高温环境对热天线电性能的影响,提出了一种热电联合计算方法,通过三维热、电信息传递程序实现不同温度区域介电性能的空间加载,以此关联温度场与电磁场网格节点信息,实现温度场-电磁场耦合问题的联合计算。介绍了热电联合计算方法的原理与思路,并以某型热天线为研究对象,考查天线温度分布对电性能的影响程度,为飞行器热天线的精细化设计提供了途径。该方法可应用于热透波结构的高温电性能分析,尤其对于恶劣热环境下的热天线/天线罩设计具有较高的应用价值。     

行星齿轮传动系统的稳态热分析

行星齿轮传动系统中,各零部件的本体温度和温度场的分布对系统的工作性能和可靠性有重要影响。以直升机的主传动系统中的行星齿轮系统为对象,建立了其发热模型和热传递模型,利用热网络分析法从而得到该系统的稳态温度分布,为行星齿轮传动系统的稳态热分析提供了一个有效的方法,并为行星齿轮系统的瞬态热分析奠定了基础     

Rheological and Thermal Properties of Icy Materials

Laboratory measurements of physical properties of planetary ices generate information for dynamical models of tectonically active icy bodies in the outer solar system. We review the methods for measuring both flow properties and thermal properties of icy planetary materials in the laboratory, and describe physical theories that are essential for intelligent extrapolation of data from laboratory to planetary conditions. This review is structured with a separate and independent section for each of the two sets of physical properties, rheological and thermal. The rheological behaviors of planetary ices are as diverse as the icy moons themselves. High-pressure water ice phases show respective viscosities that vary over four orders of magnitude. Ices of CO₂, NH₃, as well as clathrate hydrates of CH₄ and other gases vary in viscosity by nearly ten orders of magnitude. Heat capacity and thermal conductivity of detected/inferred compositions in outer solar system bodies have been revised. Some low-temperature phases of minerals and condensates have a deviant thermal behavior related to paramount water ice. Hydrated salts have low values of thermal conductivity and an inverse dependence of conductivity on temperature, similar to clathrate hydrates or glassy solids. This striking behavior may suit the dynamics of icy satellites.     

高速飞行器翼面结构热振动试验的TARMA模型方法

高速飞行器翼面结构的热振动试验研究对这类飞行器的设计和安全飞行具有重要的意义。采用时变自回归滑动平均(TARMA)模型方法建立了受热时变结构系统模态频率辨识的数学模型,并用一个数值算例进行了验证。将地面振动测试系统与瞬态热环境模拟系统相结合,设计了翼面结构热振动试验系统并模拟结构的瞬态温度场,同时对纯随机激振力激励下受热时变结构系统的振动位移信号进行测量,并用TARMA模型对时变固有频率进行了辨识,获得了前4阶固有频率随加热时间的变化规律,并将辨识结果与数值计算结果进行了比较,两者误差在5%以内。另外,在稳态均匀热环境下辨识得到的结构系统固有频率变化与数值计算结果也吻合得很好。通过将均匀温度场与瞬态温度场下的结果进行对比分析,指出了瞬态热环境下时变结构的固有频率随加热时间变化的趋势主要由结构材料属性的退化和结构内部不均匀热应力的影响共同决定。     

Planetary Magnetic Fields: Achievements and Prospects

The past decade has seen a wealth of new data, mainly from the Galilean satellites and Mars, but also new information on Mercury, the Moon and asteroids (meteorites). In parallel, there have been advances in our understanding of dynamo theory, new ideas on the scaling laws for field amplitudes, and a deeper appreciation on the diversity and complexity of planetary interior properties and evolutions. Most planetary magnetic fields arise from dynamos, past or present, and planetary dynamos generally arise from thermal or compositional convection in fluid regions of large radial extent. The relevant electrical conductivities range from metallic values to values that may be only about one percent or less that of a typical metal, appropriate to ionic fluids and semiconductors. In all planetary liquid cores, the Coriolis force is dynamically important. The maintenance and persistence of convection appears to be easy in gas giants and ice-rich giants, but is not assured in terrestrial planets because the quite high electrical conductivity of an iron-rich core guarantees a high thermal conductivity (through the Wiedemann-Franz law), which allows for a large core heat flow by conduction alone. This has led to an emphasis on the possible role of ongoing differentiation (growth of an inner core or “snow”). Although planetary dynamos mostly appear to operate with an internal field that is not very different from (2ρΩ/σ)^1/2 in SI units where ρ is the fluid density, Ω is the planetary rotation rate and σ is the conductivity, theoretical arguments and stellar observations suggest that there may be better justification for a scaling law that emphasizes the buoyancy flux. Earth, Ganymede, Jupiter, Saturn, Uranus, Neptune, and probably Mercury have dynamos, Mars has large remanent magnetism from an ancient dynamo, and the Moon might also require an ancient dynamo. Venus is devoid of a detectable global field but may have had a dynamo in the past. Even small, differentiated planetesimals (asteroids) may have been capable of dynamo action early in the solar system history. Induced fields observed in Europa and Callisto indicate the strong likelihood of water oceans in these bodies. The presence or absence of a dynamo in a terrestrial body (including Ganymede) appears to depend mainly on the thermal histories and energy sources of these bodies, especially the convective state of the silicate mantle and the existence and history of a growing inner solid core. As a consequence, the understanding of planetary magnetic fields depends as much on our understanding of the history and material properties of planets as it does on our understanding of the dynamo process. Future developments can be expected in our understanding of the criterion for a dynamo and on planetary properties, through a combination of theoretical work, numerical simulations, planetary missions (MESSENGER, Juno, etc.) and laboratory experiments.     

斜齿行星齿轮传动系统振动模式与动载特性

斜齿行星传动在高速重载场合中应用越来越广泛,其振动模式和动载特性研究对减振降噪设计具有重要意义.针对斜齿行星齿轮传动系统,建立了随动坐标系,推导了含陀螺效应的多自由度间隙非线性动力学方程,求解了系统的固有特性.结果表明:斜齿行星齿轮系统存在3种典型振动模式,即轴向平移-扭转耦合振动模式(重根数r=1),径向平移振动模式(重根数r=2)和行星轮振动模式(重根数r=N－3,N>3);综合考虑啮合刚度、齿侧间隙、综合误差和外载荷等激励作用,研究了啮合相位差和激励方式对动载系数的影响规律,结果表明计入啮合相位差时动载系数有所增大,当刚度波动系数ζ=1.723时,系统分岔为2周期次谐响应,随着激励参数的变化,内啮合较外啮合更快的进入混沌状态.      

Interior Evolution of Mercury

The interior evolution of Mercury—the innermost planet in the solar system, with its exceptional high density—is poorly known. Our current knowledge of Mercury is based on observations from Mariner 10’s three flybys. That knowledge includes the important discoveries of a weak, active magnetic field and a system of lobate scarps that suggests limited radial contraction of the planet during the last 4 billion years. We review existing models of Mercury’s interior evolution and further present new 2D and 3D convection models that consider both a strongly temperature-dependent viscosity and core cooling. These studies provide a framework for understanding the basic characteristics of the planet’s internal evolution as well as the role of the amount and distribution of radiogenic heat production, mantle viscosity, and sulfur content of the core have had on the history of Mercury’s interior. The existence of a dynamo-generated magnetic field suggests a growing inner core, as model calculations show that a thermally driven dynamo for Mercury is unlikely. Thermal evolution models suggest a range of possible upper limits for the sulfur content in the core. For large sulfur contents the model cores would be entirely fluid. The observation of limited planetary contraction (∼1–2 km)—if confirmed by future missions—may provide a lower limit for the core sulfur content. For smaller sulfur contents, the planetary contraction obtained after the end of the heavy bombardment due to inner core growth is larger than the observed value. Due to the present poor knowledge of various parameters, for example, the mantle rheology, the thermal conductivity of mantle and crust, and the amount and distribution of radiogenic heat production, it is not possible to constrain the core sulfur content nor the present state of the mantle. Therefore, it is difficult to robustly predict whether or not the mantle is conductive or in the convective regime. For instance, in the case of very inefficient planetary cooling—for example, as a consequence of a strong thermal insulation by a low conductivity crust and a stiff Newtonian mantle rheology—the predicted sulfur content can be as low as 1 wt% to match current estimates of planetary contraction, making deep mantle convection likely. Efficient cooling—for example, caused by the growth of a crust strongly in enriched in radiogenic elements—requires more than 6.5 wt% S. These latter models also predict a transition from a convective to a conductive mantle during the planet’s history. Data from future missions to Mercury will aid considerably our understanding of the evolution of its interior.     

Semi-analytic Solution of Steady Temperature Fields During Thin Plate Welding

Usually, it is very difficult to find out an analytical solution to thermal conduction problems during high temperature welding. Therefore, as an important numerical approach, the method of lines (MOLs) is introduced to solve the temperature field characterized by high gradients. The basic idea of the method is to semi-discretize the governing equation of the problem into a system of ordinary dif-ferential equations (ODEs) defined on discrete lines by means of the finite difference method, by which the thermal boundary condition with high gradients are directly embodied in formulation. Thus the temperature field can be obtained by solving the ODEs. As a numeri-cal example, the variation of an axisymmetrical temperature field along the plate thickness can be obtained.     

The Geology of Mercury: The View Prior to the MESSENGER Mission

Mariner 10 and Earth-based observations have revealed Mercury, the innermost of the terrestrial planetary bodies, to be an exciting laboratory for the study of Solar System geological processes. Mercury is characterized by a lunar-like surface, a global magnetic field, and an interior dominated by an iron core having a radius at least three-quarters of the radius of the planet. The 45% of the surface imaged by Mariner 10 reveals some distinctive differences from the Moon, however, with major contractional fault scarps and huge expanses of moderate-albedo Cayley-like smooth plains of uncertain origin. Our current image coverage of Mercury is comparable to that of telescopic photographs of the Earth’s Moon prior to the launch of Sputnik in 1957. We have no photographic images of one-half of the surface, the resolution of the images we do have is generally poor (∼1 km), and as with many lunar telescopic photographs, much of the available surface of Mercury is distorted by foreshortening due to viewing geometry, or poorly suited for geological analysis and impact-crater counting for age determinations because of high-Sun illumination conditions. Currently available topographic information is also very limited. Nonetheless, Mercury is a geological laboratory that represents (1) a planet where the presence of a huge iron core may be due to impact stripping of the crust and upper mantle, or alternatively, where formation of a huge core may have resulted in a residual mantle and crust of potentially unusual composition and structure; (2) a planet with an internal chemical and mechanical structure that provides new insights into planetary thermal history and the relative roles of conduction and convection in planetary heat loss; (3) a one-tectonic-plate planet where constraints on major interior processes can be deduced from the geology of the global tectonic system; (4) a planet where volcanic resurfacing may not have played a significant role in planetary history and internally generated volcanic resurfacing may have ceased at ∼3.8 Ga; (5) a planet where impact craters can be used to disentangle the fundamental roles of gravity and mean impactor velocity in determining impact crater morphology and morphometry; (6) an environment where global impact crater counts can test fundamental concepts of the distribution of impactor populations in space and time; (7) an extreme environment in which highly radar-reflective polar deposits, much more extensive than those on the Moon, can be better understood; (8) an extreme environment in which the basic processes of space weathering can be further deduced; and (9) a potential end-member in terrestrial planetary body geological evolution in which the relationships of internal and surface evolution can be clearly assessed from both a tectonic and volcanic point of view. In the half-century since the launch of Sputnik, more than 30 spacecraft have been sent to the Moon, yet only now is a second spacecraft en route to Mercury. The MESSENGER mission will address key questions about the geologic evolution of Mercury; the depth and breadth of the MESSENGER data will permit the confident reconstruction of the geological history and thermal evolution of Mercury using new imaging, topography, chemistry, mineralogy, gravity, magnetic, and environmental data.     

行星齿轮非线性振动系统参数稳定域的计算方法

研究了行星齿轮非线性传动系统参数稳定域计算的一般方法.该方法通过选取合理的失稳阀值,根据考查参数域内系统的运动状态选取合适的数值积分时间段,以循环套嵌的手段计算考查参数在各自范围内不同组合下的系统位移响应最大值,比较失稳阀值以判稳,参数稳定域的图形输出等5个步骤完成对行星轮系参数稳定域的计算.最后,以四自由度行星轮系纯扭转非线性振动模型为例,以行星轮输入转速、系统的齿侧间隙以及齿轮副的啮合阻尼系数为考查参数,分别计算得到了系统的单参数稳定域、双参数稳定域以及三参数稳定域,为行星轮系的设计取值提供了重要参考.