智能赋能流体力学展望

人工智能（AI）是21世纪的前沿科技,流体力学如何在智能化时代焕发青春是值得本领域研究者思考的话题。从智能赋能流体力学角度,就其研究内涵、研究内容、近期研究及难点进行了总结,并对智能流体力学未来的发展进行了展望。研究指出,流体力学计算或试验中所产生的数据是天生的大数据,如何通过深度神经网络、随机森林、强化学习等机器学习方法来利用这些数据,缓解甚至替代理论和方法层面对人脑的依赖,挖掘新的知识,成为一种新的研究范式;相关研究将涵盖流动控制方程的机器学习、湍流模型的机器学习、物理量纲分析与标度的智能化以及数值模拟方法的智能化;借助人工智能技术,发展流动信息特征提取与多源数据融合的智能化是流体力学发展的迫切需求;研究内容应至少涵盖海量数据挖掘方法以及多源气动数据的智能融合;发展数据驱动的流体力学多学科、多物理场耦合建模与控制是工程应用的迫切需求,相关工作涉及多场耦合建模、气动外形智能优化设计以及流动智能自适应控制等方面。     

湍流数据同化技术及应用

近年来数据同化（DA）被引入湍流动力学研究中,通过融合实验测量和数值计算,提高了实验测量的精度和广度,改善了数值模拟的预测性能。实验观测、预测模型和同化算法是数据同化的三要素,湍流研究中的实验观测包括热线风速仪、粒子图像测速法（PIV）、压力传感器等局部测量数据,预测模型主要指流动控制方程及湍流封闭方程,而同化算法包括贝叶斯推断、集合卡尔曼滤波（EnKF）、伴随等。稳态数据同化一般结合雷诺平均Navier-Stokes （RANS）模型方程,从重新标定模型常数、修正涡黏模型方程形式误差、修正雷诺应力项等方面着手。非稳态的数据同化一般包括四维变分（4DVar）等时间连续的数据同化方式以及顺序数据同化。4DVar通过时间正向和逆向积分迭代,存储量和计算量都非常大。顺序数据同化不需要时间逆向积分,可以在若干时刻对实验观测进行间断地植入,正向求解整个系统。另外,随着人工智能的飞速发展,湍流数据同化研究也向智能化迈进。对于纯数据驱动的湍流机器学习,其缺乏物理本质的约束,而基于物理信息的机器学习在物理本质上与数据同化是一致的。     

人工智能技术在航空发动机孔探检测中的应用进展

孔探是当前航空发动机检修过程中应用最多的无损检测方法,也是孔探图像的唯一获取途径。近年来,深度学习等人工智能方法开始被应用到航空发动机损伤分类、检测中,为实现航空发动机检修智能化提出了一些现行有效的方法,具有重要的工业应用价值。本文概述了航空发动机孔探检测的发展和优缺点,综述了专家系统和机器学习人工智能方法在发动机孔探图像方面的应用进展,总结了基于孔探图像实现航空发动机孔探检测智能化面临的一些挑战。     

机器学习辅助湍流建模在分离流预测中的应用

数据驱动湍流建模是近年来发展的提高雷诺平均N-S方程预测精度的有效手段,通过机器学习算法能够从高置信度数据中自动提取特征,建立准确的从平均流动特征到雷诺应力的预测模型。针对高雷诺数下积冰翼型绕流这一类典型的复杂流动分离问题,基于此前研究者提出的机器学习预测框架,从输入输出特征选择和翼型绕流中数据分布特性两个方面出发,对机器学习预测结果的光滑性和准确性进行改善。提出了基于雷诺应力张量分析和流动特征辨识的输入特征选择准则;提出了局部区域建模方法以及基准模型和机器学习预测模型混合的代入计算方法。将改进方法应用于积冰翼型绕流问题之中,结果表明改进的方法能够准确给出训练集和预测集上的雷诺应力结果,并且代入平均流计算可以得到和真实分布更加接近的流动和机翼表面压力分布。     

发动机湍流燃烧多物理耦合建模和仿真进展

航空发动机燃烧室喷雾燃烧包含液滴破碎、雾化、蒸发、掺混、燃烧等多个物理过程,各物理过程相互耦合,产生出预混、非预混、自着火等多种燃烧模式,不同的燃烧模式表现出的湍流-化学反应相互作用也各不相同,对发展普适的湍流燃烧模型提出了巨大挑战。针对多物理场耦合的湍流燃烧过程进行物理建模成为湍流燃烧建模研究的主要任务之一。此外,航空发动机湍流燃烧研究也面对着工程设计和优化的客观需求,即发展效率和精度兼顾的高效湍流燃烧仿真方法并量化湍流燃烧控制物理机制,为燃烧组织调控提供指导。综合上述内容,从发动机两相喷雾燃烧模式、自适应燃烧建模和主控物理机制分析等方面点评和回顾了近期的基础研究进展,对当前的研究现状做了初步总结。     

航空发动机风扇宽频噪声预测技术发展研究

综述了风扇宽频噪声预测技术在航空发动机噪声控制领域的研究进展和应用,包括经验模型、分析模型、计算气动声学和机器学习等方法。对这些方法的发展现状进行了回顾,并对国内外情况进行了对比分析。研究发现,不同的预测模型适用于不同阶段的设计过程,如经验模型适用于概念设计阶段,分析模型适用于通流设计阶段,计算气动声学适用于详细设计阶段。此外,基于机器学习的风扇尾迹湍流预测是一个重要的研究方向,提高训练效率和预测精度将显著提升机器学习的适用性。最后,对风扇宽频噪声预测方法进行了简要总结和展望。     

航空航天CFD物理模型和计算方法的述评与挑战

CFD(computational fluid dynamics)在航空航天中的应用发展迅速、成效斐然,成为飞行器研制和空气动力学研究的重要手段。但另一方面,CFD在物理模型和计算方法等核心理论上的进步却显得步履蹒跚。为此,本文聚焦CFD在航空航天中的应用,从湍流模型、转捩模型、通量求解方法以及高阶格式等CFD关键问题评述其发展现状及面临的挑战。在湍流模型中,重点论述了常用的线性涡黏性模型的现状和特性,尤其是其不足,对比分析了更复杂的雷诺应力模型。在转捩模型中,主要包括低雷诺数湍流模型、间歇因子转捩模型和层流动能转捩模型等,重点介绍了各类模型的发展历程、构造方式和适用范围。在通量求解方法中,重点关注迎风通量格式,论述其在解决激波异常、overheating、全速域模拟、多维流动等问题方面的发展现状。在高阶格式中,主要关注WENO和DG等格式,论述其在计算精度、时间求解、激波捕捉、计算效率等性能方面的现状和问题。最后针对上述方向给出了简要总结和未来发展的建议等。     

人工智能在航天器制导与控制中的应用综述

航天器制导与控制技术是保障空间任务顺利实施的关键技术之一。当前,动力学模型的强非线性以及参数不确定性制约了高精度姿轨控技术的发展,而系统故障则决定航天器姿轨控的成败。以机器学习为代表的新一代人工智能技术航天器制导控制领域展现了巨大的应用潜力。首先对基于人工智能技术的轨迹制导和姿态控制中的研究发展及应用现状进行归纳,分析航天器轨迹规划、姿态控制、故障诊断以及容错控制技术的发展趋势。然后,从鲁棒轨迹规划、自适应姿态控制、快速故障诊断和自适应容错控制等4个方面总结适用于未来航天任务的航天器姿轨控关键技术。最后,针对智能姿轨控技术的应用所面临的挑战,从姿轨控架构、算法最优性、算法的训练以及技术验证等方面提出相应的发展建议。     

超声速燃烧数值模拟中的湍流与化学反应相互作用模型

高精度数值模拟有助于理解超声速湍流燃烧中湍流与化学反应的相互作用,可为发动机燃烧室等工程应用设计提供可靠的预测模型。除直接数值模拟外,目前在湍流燃烧应用中使用的大涡模拟和雷诺平均Navier-Stokes模拟均需要借助模型模化发生在湍流小尺度上的流动与化学反应过程对湍流大尺度运动的影响。现有的湍流与化学反应相互作用模型大致可分为:火焰面类模型和概率密度函数类模型,2类模型在不同的应用中各自具有优势和局限性。此外,现有模型大都基于低马赫数燃烧,而超声速燃烧中通常会伴随快速混合、局部熄火和再着火以及激波等复杂过程,这为发展其中的湍流与化学反应相互作用模型提出了更多的挑战。     

基于机器学习的单孔绝热气膜冷却效率分布预测研究

为了研究利用机器学习技术对绝热冷却效率进行直接预测的方法及特点,搭建了基于上采样卷积神经网络的机器学习模型,生成了用于训练以及验证的数值模拟数据集,使用了监督式学习的方法对模型进行了训练.训练使用反向传播算法和基于随机梯度下降的Adam优化算法,输入模型的参数包括吹风比、主流湍流强度、喷射角、孔形状、孔尺寸,模型输出为...     

Isotopic Abundances in Comets

Isotopic ratios in comets provide keys for the understanding of the origin of cometary material, and the physical and chemical conditions in the early Solar Nebula. We review here measurements acquired on the D/H, ¹²C/¹³C, ¹⁶O/¹⁸O, ¹⁴N/¹⁵N, ³²S/³⁴S ratios in dust and gases, and discuss their cosmogonic implications. The prospects for future measurements from cometary space missions and remote sensing observations at millimeter and submillimeter wavelengths are presented. This revised version was published online in August 2006 with corrections to the Cover Date.     

Alfvénic Electron Acceleration in Aurora Occurs in Global Alfvén Resonosphere Region

Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science 299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of 4–5 R _E (Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is responsible for the energy transfer.     

Space Weather Research in China

Recent progress in space weather research are briefly presented here from three aspects: establishment or improvement in observation systems, such as extra-soft X-ray detector and γ-ray detector onboard the spacecraft ‘Shen Zhou 2’, new solar radio broad-band spectrometer, magnetometer-chain, ionosonde and digisonde–chain, laser-lidar system and VHF radar; partial topic progresses included in CMEs, multi-streamer structures, evolution of interplanetary magnetic field B _z component, regional properties of traveling ionospheric disturbances, a fully-nonlinear global dynamical model for the middle and upper atmosphere, and a combined prediction method for geomagnetic disturbances; and space weather activity, such as ‘Meridian Project’ — a national major scientific project, ‘International Space Weather Meridian Circle Program’ — a suggestion of internationalization of ‘Meridian Project’, ‘Space Weather Research Plan’ — a major research plan from National Natural Science Foundation of China (NNSFC) and other space weather activities. This revised version was published online in August 2006 with corrections to the Cover Date.     

Deuterium Fractionation in Interstellar Clouds

This paper reviews the chemical processes responsible for fractionating deuterium in interstellar molecules. I show that this process is intrinsically a low temperature phenomenon and discuss how the degree of enhancement of the deuterium content of molecules is related to the physical conditions, particularly abundances, in molecular clouds. If significant amounts of abundant species, such as CO, are frozen out on to interstellar dust grains, the resulting enhancement in H₂D⁺ can result in its abundance being greater than that of H ₃ ⁺ at 10K. Transfer of the deuteron from H₂D⁺ can then lead to the efficient formation of multiply deuterated species, such as NHD₂ and ND₃. Fractionation can also occur in grain surface reactions and some simple models are discussed. This revised version was published online in August 2006 with corrections to the Cover Date.     

Element Abundances in X-ray Emitting Plasmas in Stars

Studies of element abundances in stars are of fundamental interest for their impact in a wide astrophysical context, from our understanding of galactic chemistry and its evolution, to their effect on models of stellar interiors, to the influence of the composition of material in young stellar environments on the planet formation process. We review recent results of studies of abundance properties of X-ray emitting plasmas in stars, ranging from the corona of the Sun and other solar-like stars, to pre-main sequence low-mass stars, and to early-type stars. We discuss the status of our understanding of abundance patterns in stellar X-ray plasmas, and recent advances made possible by accurate diagnostics now accessible thanks to the high resolution X-ray spectroscopy with Chandra and XMM-Newton.     

Electric gaps in pulsar magnetospheres

Two contrasting models of the magnetosphere are studied: a classical, quasi-mhd model, in which it is the componentE that accelerates electrons to relativistic energies; and a model with e⁺-e^– production, in which the componentE is locally crucial, both in an acceleration domain near the star and in a dissipation domain beyond the light-cylinder.     

Helium in the terrestrial atmosphere

After a brief historical review of the discovery of helium in the terrestrial atmosphere, the production mechanisms of the isotopes He⁴ and He³ are discussed. Although the radioactive production of He⁴ in the Earth is well understood, some uncertainty still exists for the degassing process leading to an atmospheric influx of (2.5 ±1.5) × 10⁶ atoms cm^–2 s^–1. Different production mechanisms are possible for He³ leading to an influx of (7.5±2.5) atoms cm^–2 s^–1. Observations of helium in the thermosphere show a great variability of this constituent. The different mechanisms proposed to explain the presence of the winter helium bulge are discussed. Since helium ions are present in the topside ionosphere and in the magnetosphere, ionization mechanisms are analyzed. Owing to possible variations and uncertainties in the solar UV flux, the photoionization coefficient is (8±4) × 10^–8 s^–1. Finally, the helium balance between production in the earth and loss into the interplanetary space is discussed with respect to the different processes which can play an effective role.     

Research on uncertainty in measurement assisted alignment in aircraft assembly

Operations in assembling and joining large size aircraft components are changed to novel digital and flexible ways by digital measurement assisted alignment.Positions and orientations（P＆O）of aligned components are critical characters which assure geometrical positions and relationships of those components.Therefore,evaluating the P＆O of a component is considered necessary and critical for ensuring accuracy in aircraft assembly.Uncertainty of position and orientation（U-P＆O）,as a part of the evaluating result of P＆O,needs to be given for ensuring the integrity and credibility of the result;furthermore,U-P＆O is necessary for error tracing and quality evaluating of measurement assisted aircraft assembly.However,current research mainly focuses on the process integration of measurement with assembly,and usually ignores the uncertainty of measured result and its influence on quality evaluation.This paper focuses on the expression,analysis,and application of U-P＆O in measurement assisted alignment.The geometrical and algebraical connotations of U-P＆O are presented.Then,an analytical algorithm for evaluating the multi-dimensional U-P＆O is given,and the effect factors and characteristics of U-P＆O are discussed.Finally,U-P＆O is used to evaluate alignment in aircraft assembly for quality evaluating and improving.Cases are introduced with the methodology.     

Magnetic field measurements in space

Conclusions The magnetosphere boundary has been penetrated in several places, conflicting evidence about the ring current location has been found, and the field exterior to the boundary has revealed some unexpected features. Pronouncements about the structure of the geomagnetic and interplanetary magnetic fields are still based on scanty evidence but the experimental basis of such estimates is more adequate than in 1958.The boundary between the geomagnetic field and the interplanetary medium has been found, by Explorer XII, to be located at approximately 10 R _E on the sunlit side of the earth near the equator. It has been observed to fluctuate between 8 and 12 R _E during August, September and October of 1961. During several days in March, 1961, the boundary, on the dark side of the earth, was penetrated repeatedly by Explorer X on an outbound pass near 135° from the earth-sun line. Several interpretations are possible; the most reasonable one at present is that the boundary was fluctuating in this period, placing the satellite alternately inside the geomagnetic field and outside in a region of turbulent magnetic fields and plasma flow.A region of turbulent magnetic fields was also observed by Pioneer I, Pioneer V, and Explorer XII between 10 and 15 R _E on the sunlit side of the earth. Pioneer V observed also a steady field 2 to 5 gammas in magnitude beyond 20 R _E. It appears that there exists a region of turbulent magnetic fields between the geomagnetic field boundary near 10 R _E, and another boundary, located near 14–15 R _E near the earth-sun line. This second boundary was seen only by Pioneer I and Pioneer V; Explorer XII and Explorer X apparently did not reach it. This boundary has been tentatively identified as a shock front in the flow of solar plasma about the magnetosphere (see Figure 5).^{41, 42} The geomagnetic field inside the boundary is relatively quiet. An abrupt transition in the magnitude of fluctuations occurs at the boundary surface. The ratio of fluctuation amplitude, B, to average field, B, decreases from 1 to 0.1 on a passage through the boundary on 13 September 1961.⁴³ The boundary is not unstable in the solar wind but fluctuations in solar wind pressure do cause changes in boundary location.^42,43 The ring current location appears to be above 1.4 R _E and below 5 R _E on the basis of Pioneer I, Vanguard III, and Explorer XII data. Lunik I and II records indicate that it is located between 3 and 4 R _E. Explorer VI data indicates that it must be at distances greater than 4 R _E on the dark side of the earth. Some variation in altitude of a ring current with time appears likely, but the bulk of present evidence limits a possible ring current to a distance of 3 to 5 R _E.The interplanetary field during quiet times is of the order of 2 to 5 gammas. The direction indicated for this field, with a significant component perpendicular to the earth-sun line, is puzzling in view of solar cosmic ray transit times. Solar disturbances with resultant plasma flow past the satellite produce increases in the field magnitude. Field increases at the satellite are sometimes correlated with disturbances observed at the earth.Further investigations are needed to map the magnetosphere and boundary more completely, to investigate the postulated shock front and the turbulent region inside, to refute or confirm the ring current theory, and to measure the interplanetary field direction and magnitude more completely. Theoretical studies are needed to support these experiments and to suggest new avenues of investigations. Particularly needed are theoretical investigations of collisionless shock fronts in plasma flow and of characteristics of the flow between the shock front and the obstacle.