Cloud Formation and the Possible Significance of Charge for Atmospheric Condensation and Ice Nuclei

Cloud formation in the atmosphere is related to the presence of water vapour, cloud condensation nuclei (CCN) and ice nuclei (IN). Ionisation in the atmosphere is caused by a variety of sources, but the contribution from cosmic rays is always present and is modulated by the solar cycle. Methods of investigating the variability in ionisation are described. The mechanisms proposed by which (1) ionisation could influence cloud formation, and (2) by which changes to the CCN and IN could occur are discussed. Direct formation of sulphate CN is conceivable in atmospheric air by radioactivity, and charging of molecular clusters leads to greater collisions rates than for neutral clusters. Modification of the ice nucleation efficiency of aerosol could also have atmospheric effects through latent heat release. However in both cases definitive atmospheric experimental work is lacking and therefore any link between solar variability and clouds remains unproven.     

云计算综述

论述了云计算的起源、概念、特点,与分布式计算和网格计算的区别;介绍了云计算厂商,及各厂商采用的数据存储、数据管理、编程模式、提供的服务种类云计算存在的问题,特别是云计算安全的风险种类及防护方法。提出了云计算需解决的问题。     

云作战条件下空天信息装备体系建设

云作战是云计算技术在军事领域带来的全新作战模式。在未来空天成体系对抗中,云作战将具有作 战力量聚散无形和作战行动虚实结合的优势。本文分析了空天信息装备体系的建设需求,基于云作战概念,构建了空天信息装备体系;从重视云作战制胜机理研究、提升装备融合能力、重视可靠性和安全性、坚持统筹协调 等角度,探讨了云作战概念对空天信息装备体系建设的启示,深化了空天信息装备体系建设需求与实现途径的 认识,对空天战场信息装备成体系建设与运用具有一定的借鉴意义。     

单光子激光雷达数据去噪与滤波算法

单光子激光雷达获取的点云数据存在大量噪声,这给数据的处理带来了挑战。基于局部距离统计提出了改进的点云去噪算法,对单光子激光雷达点云原始数据进行去噪。然后基于统计分析方法改进了点云滤波算法,对去噪后的点云数据进行滤波处理。利用新提出的算法与传统算法去噪和滤波后得到的点云进行比较,并与传统激光雷达的数字地形模型(DTM)数据进行对比。计算得到MABEL地面点云相对于传统激光雷达高程的均方根误差RMSE为2.98m,相关系数R^2为0.9938。进一步对地面点云插值得到剖面数字高程模型(DEM)数据,其相对于传统激光雷达高程的均方根误差RMSE为2.85m,相关系数R^2为0.9931。实验结果显示,提出的单光子激光雷达点云去噪和滤波算法优于传统算法,与传统激光雷达DTM数据具有较好的相关性,能够精确的恢复地形信息。     

永磁同步电机的自适应云模型控制研究

针对PID或其改进的算法鲁棒性偏低问题,提出了永磁同步电机(PMSM)的自适应云模型控制算法研究。在分析了自适应云模型结构后设计了PMSM自适应云模型控制器。搭建了基于自适应云模型控制算法的PMSM试验平台,试验结果表明提出的PMSM的自适应云模型控制算法精度高、性能稳定。     

Aerosol-Cloud Interactions Control of Earth Radiation and Latent Heat Release Budgets

Aircraft observations and model simulations show that cloud development is strongly modulated by the impact of cloud-aerosol interactions on precipitation forming processes. New insights into the mechanisms by which aerosols dominate the cloud cover of marine shallow clouds suggest that feedbacks between the cloud microstructure and cloud dynamics through precipitation processes play a major role in determining when a solid cloud cover will break up into a field of trade wind cumulus. Cloud-aerosol interactions dominate not only the dynamics of marine shallow clouds, but also the lifetime and the vertical disposition of latent heat of deep convective clouds over ocean and even more strongly over land. Recent coincident satellite measurements of aerosols and cloud properties quantify the aerosol effects on cloud cover and radiative forcing on regional and global scales. The shapes of the satellite retrieved relations between aerosols and cloud properties are consistent with the suggested ways by which aerosols affect clouds via precipitation processes, particularly by affecting the intensity of the cloud vertical air motions and its vertical development.     

Triggering Protostellar Collapse, Injection, and Disk Formation

Certain meteoritical inclusions contain evidence for the existence of short-lived radioactivities such as ²⁶Al and ⁴¹Ca at the time of their formation 4.566 billion years ago. Because the half-lives of these nuclides are so short, this evidence requires that no more than about a million years elapsed between their nucleosynthesis and their inclusion in cm-sized solids in the solar nebula. This abbreviated time span can be explained if these nuclides were synthesized in a stellar source such as a supernova, and were then transported across the interstellar medium by the resulting shock wave, which then triggered the gravitational collapse of the presolar molecular cloud core. Detailed 2D and 3D numerical hydrodynamical models are reviewed and show that such a scenario is consistent with the time scale constraint, and with the need to both trigger collapse and to inject shock-wave matter into the collapsing protostellar cloud and onto the protoplanetary disk formed by the collapse. This revised version was published online in June 2006 with corrections to the Cover Date.     

OpenGVS中三维云的快速模拟

三维云的模拟可以大大提高飞行模拟器视景的逼真度,粒子系统又是模拟三维云的有效方法.介绍了三维视景中模拟三维云的几种常用方法,分析了OpenGVS中仿真云的局限性以及粒子系统模拟三维云的优点,在分析粒子系统的基础上,提出了一种在OpenGVS中基于灰度图约束的模拟三维云的方法,利用该算法,通过恰当选择粒子数量和粒子模型可以在取得逼真效果的同时满足视景系统实时性的要求.最后给出了在OpenGVS中的实现方法.     

The relevance of molecular observations to gamma-ray astronomy

The interaction of cosmic rays with interstellar clouds may produce some of the observed gamma-ray sources. The use of molecular observations to estimate the cloud masses, which are used to derive cosmic-ray fluxes, is reviewed. Molecular diagnostics of high cosmic-ray ionization rates are discussed, and a detailed application of those diagnostics is summarised and presented as evidence that second-order Fermi acceleration is important in old supernova remnants and can produce cosmic rays of too low energy to induce gamma-ray emission.Proceedings of the XVIII General Assembly of the IAU: Galactic Astrophysics and Gamma-Ray Astronomy, held at Patras, Greece, 19 August 1982.Royal Society Jaffé Donation Fellow.     

Experimental and numerical study of chaff cloud kinetic performance under impact of high speed airflow

To solve the kinetic and diffusion problem of surface-type infrared decoy, multi-chaff kinetic models are established and chaff cloud holistic kinetic performance are analyzed under the impact of high speed airflow in this work. Chaffs rotate rapidly during the motion under the impact of high speed airflow. The rotation speed is correlated with lift, position of pressure center and aerodynamic damping. Computational Fluid Dynamics (CFD) is used to compute the aerodynamic coefficients of chaff. It is found that there exists serious aerodynamic interference which mainly relates to the overlapping area and distance among chaffs during the diffusion of chaff cloud. The chaff wind tunnel test and rocket sled experiment are carried out to verify the credibility of the models in this work. Then, the variation of chaff cloud expectation and extremum are analyzed to achieve the holistic kinetic and diffusing performance of chaff cloud. Simulation results demonstrate that the chaffs diffuse rapidly under the impact of high speed airflow and chaff cloud can be formed rapidly within 0.5?s. The shape of the chaff cloud is similar to cone that forms a certain angle with the horizontal plane and most chaffs focus on the second half.     

Interstellar Matter and the Boundary Conditions of the Heliosphere

The interstellar cloud surrounding the solar system regulates the galactic environment of the Sun, and determines the boundary conditions of the heliosphere. Both the Sun and interstellar clouds move through space, so these boundary conditions change with time. Data and theoretical models now support densities in the cloud surrounding the solar system of n(H0)=0.22±0.06 cm−3, and n(e−)∼0.1 cm−3, with larger values allowed for n(H0) by radiative transfer considerations. Ulysses and Extreme Ultraviolet Explorer satellite He0 data yield a cloud temperature of 6400 K. Nearby interstellar gas appears to be structured and inhomogeneous. The interstellar gas in the Local Fluff cloud complex exhibits elemental abundance patterns in which refractory elements are enhanced over the depleted abundances found in cold disk gas. Within a few parsecs of the Sun, inconclusive evidence for factors of 2–5 variation in Mg+ and Fe+ gas phase abundances is found, providing evidence for variable grain destruction. In principle, photoionization calculations for the surrounding cloud can be compared with elemental abundances found in the pickup ion and anomalous cosmic-ray populations to model cloud properties, including ionization, reference abundances, and radiation field. Observations of the hydrogen pile up at the nose of the heliosphere are consistent with a barely subsonic motion of the heliosphere with respect to the surrounding interstellar cloud. Uncertainties on the velocity vector of the cloud that surrounds the solar system indicate that it is uncertain as to whether the Sun and α Cen are or are not immersed in the same interstellar cloud. This revised version was published online in June 2006 with corrections to the Cover Date.     

Galaxies in a Box: A Simulated View of the Interstellar Medium

We review progress in the development of physically realistic three dimensional simulated models of the galaxy. We consider the scales from star forming molecular clouds to the full spiral disc. Models are computed using hydrodynamic (HD) or magnetohydrodynamic (MHD) equations and may include cosmic ray or tracer particles. The dynamical scales covered, ranging from the full galaxy structure, through the turbulent scales of supernova (SN) explosions, down to cloud collapse and star formation, make it impossible with current computing tools and resources to resolve all of these in one model. We therefore consider a hierarchy of models and how they can be related to enhance our understanding of the complete galaxy.     

结冰风洞中过冷大水滴云雾演化特性数值研究

为明晰结冰风洞中过冷大水滴（SLD）云雾演化特性,发展了基于欧拉法的SLD液滴运动、传热和传质耦合计算方法,针对3 m×2 m结冰风洞主试验段水平收缩构型,分析了SLD云雾沉降收缩特性、动量平衡特性和热平衡特性,探索了液滴变形破碎的影响,评估了构型出口处SLD液滴动量平衡和热平衡状态。研究结果表明：直径超过250 μm的SLD液滴在构型内会发生显著形变,液滴尺寸越大则变形程度越强,尤其在160 m/s工况下,当液滴直径超过750 μm后,SLD液滴甚至会发生破碎;液滴变形破碎效应会增大液滴加速度和液滴温度下降率,促使SLD液滴趋近动量平衡和热平衡状态;SLD云雾（最大液滴直径小于1 000 μm）在构型出口处会出现显著的粒径浓度分层、动量分层和热分层现象,其中直径小于100 μm的小尺寸液滴速度快、温度低且不断凝结,趋于平衡态,但直径超过500 μm的大尺寸SLD液滴速度慢、温度高且不断蒸发,则显著偏离平衡态;增大试验段气流速度尽管会减弱SLD云雾粒径浓度分层程度,但会增强动量分层和热分层程度,尤其在160 m/s工况下,SLD云雾会均匀分布在构型出口中心区域内（-0.75 m < Y < 0.75 m且-0.5 m < Z < 0.5 m）,与其平衡态间的最大速度差和温度差将分别超过18 m/s和20℃。     

The clouds of Venus

The current state of knowledge of the Venusian clouds is reviewed. The visible clouds of Venus are shown to be quite similar to low level terrestrial hazes of strong anthropogenic influence. Possible nucleation and particle growth mechanisms are presented. The Pioneer Venus experiments that emphasize cloud measurements are described and their expected findings are discussed in detail. The results of these experiments should define the cloud particle composition, microphysics, thermal and radiative heat budget, rough dynamical features and horizontal and vertical variations in these and other parameters. This information should be sufficient to initialize cloud models which can be used to explain the cloud formation, decay, and particle life cycle.     

一种能量级自然云雷达图像仿真方法

针对飞行模拟训练需求,基于自然云与电磁波束相互作用的统计特性,设计了 1种自然云雷达图像仿真方案,给出了多个关键仿真模型的实现方法。通过雷达波束的子波束划分实现雷达波束充塞系数的估算,解决了波束充塞系数计算难度大的问题,并根据云的三维模型设计了雷达回波能量计算模型。通过将三维空间的计算转化到二维平面内以获取雷达波束中心与云团交点位置及参数,以此计算雷达反射率和雷达回波的距离衰减。仿真实验表明:该方法能较好地体现云对回波的衰减效应,以及波束充塞度对远距离云回波计算的影响,具有较好的实时性。     

Bistatic Radar Cross Sections of Horizontally Oriented Chaff

Bistatic radar cross sections are determined for scattering from a cloud of randomly positioned resonant dipoles (chaff). Dipoles are assumed to be horizontally oriented with axes randomly oriented in the horizontal plane. The cloud is arbitrarily located relative to an illuminating source having an arbitrary (elliptical) polarization. Cloud cross section is found for an arbitrarily located receiver that views the cloud with an antenna of arbitrary polarization. Cross section applicable to the receiver's orthogonal polarization is also found.     

基于云关联度的航空发动机传感器、部件故障识别系统设计

针对灰色关联度方法用于发动机故障诊断精度低的问题,结合云理论和关联度分析方法,提出了云关联度方法,利用“云滴”能够反映映射的模糊性和随机性与整体“形状”变化分布这一特性,克服数据挖掘的模糊性和随机性问题,采用综合隶属度方法能够充分对数据进行挖掘,最终计算出云关联度.为了实现航空发动机传感器、部件单一故障的实时识别和诊断,在分析航空发动机传感器故障和部件故障特点的基础上,利用云关联度方法,设计了航空发动机传感器、部件故障的识别系统.仿真结果表明该方法不仅能够实时正确区分航空发动机传感器、部件故障,还能准确诊断出故障发生的传感器或者部件的位置,有效地改善了航空发动机故障诊断能力.      

航空发动机健康管理云服务系统设计与实现

为提高航空公司的资源利用率和经营管理水平,设计了一个基于云计算的航空发动机健康管理系统。分析了航空公司对云服务系统的需求,介绍了系统的结构体系和系统开发和运行的环境。叙述了系统的功能模型和信息模型,并通过发动机健康管理一个模块——“水洗”的使用来说明系统的使用过程。     

Evolution of the Protosolar Nebula and Formation of the Giant Planets

The formation of planetary systems is intimately tied to the question of the evolution of the gas and solid material in the early nebula. Current models of evolution of circumstellar disks are reviewed here with emphasis on the so-called “alpha models” in which angular momentum is transported outward by turbulent viscosity, parameterized by an dimensionless parameter α. A simple 1D model of protoplanetary disks that includes gas and embedded particles is used to introduce key questions on planetesimal formation. This model includes the aerodynamic properties of solid ice and rock grains to calculate their migration and growth. We show that the evolution of the nebula and migration and growth of its solids proceed on timescales that are generally not much longer than the timescale necessary to fully form the star-disk system from the molecular cloud. Contrary to a widely used approach, planet formation therefore can neither be studied in a static nebula nor in a nebula evolving from an arbitrary initial condition. We propose a simple approach to both account for sedimentation from the molecular cloud onto the disk, disk evolution and migration of solids. Giant planets have key roles in the history of the forming Solar System: they formed relatively early, when a significant amount of hydrogen and helium were still present in the nebula, and have a mass that is a sizable fraction of the disk mass at any given time. Their composition is also of interest because when compared to the solar composition, their enrichment in elements other than hydrogen and helium is a witness of sorting processes that occured in the protosolar nebula. We review likely scenarios capable of explaining both the presence of central dense cores in Jupiter, Saturn, Uranus and Neptune and their global composition. This revised version was published online in August 2006 with corrections to the Cover Date.     

基于局部几何特征的稠密点云配准方法

针对现有的稠密点云配准方法依赖初始位置设定、计算成本高、配准成功率不高等问题，提出了一种基于点云局部几何特征的稠密点云配准方法。采用深度卷积网络模型提取点云的局部几何特征，从而减少了三维点云数据的噪声、低分辨率和不完备性等带来的影响。在此基础上，使用K维树搜索完成局部几何特征描述子的关联工作。最后，通过随机采样一致算法对点云的相对位姿进行鲁棒的估计。通过对开源数据集上5个典型场景中的数据测试表明，该方法的配准成功率达到92.5%，配准精度达到0.0434m，配准时间相对最邻点迭代配准算法缩短了74.7%，实验结果验证了该方法的有效性、实时性和鲁棒性。