Investigation of the differential rotation of the large-scale magnetic elements for the solar activity cycles 20 and 21

The differential rotation of the patterns of the large-scale solar magnetic field during solar activity cycles 20 and 21 is investigated. Compact magnetic elements with the polarity of the general solar magnetic field have larger speed of rotation than the elements with the opposite polarity. The surface of the Sun was divided by 10°-zones. In all of them the average rotation rate of the magnetic elements with negative polarity is little higher than that of the magnetic elements with positive polarity, except for 50°-zone of the south hemisphere and at the 10° latitude of the north hemisphere.

The rates of differential rotation for large-scale magnetic elements with negative and positive polarities have similar behavior for both cycles of the solar activity.

The rotation rate varies at polarity reversal of the circumpolar magnetic fields. For the cycle No 20 in 1969–1970 the threefold reversal took place in the northern hemisphere and variations of rotation rate can be noticed for magnetic elements both with positive and negative polarity for each 10°-zone in the same hemisphere.     

Simulation Techniques for Cosmological Simulations

Modern cosmological observations allow us to study in great detail the evolution and history of the large scale structure hierarchy. The fundamental problem of accurate constraints on the cosmological parameters, within a given cosmological model, requires precise modelling of the observed structure. In this paper we briefly review the current most effective techniques of large scale structure simulations, emphasising both their advantages and shortcomings. Starting with basics of the direct N-body simulations appropriate to modelling cold dark matter evolution, we then discuss the direct-sum technique GRAPE, particle-mesh (PM) and hybrid methods, combining the PM and the tree algorithms. Simulations of baryonic matter in the Universe often use hydrodynamic codes based on both particle methods that discretise mass, and grid-based methods. We briefly describe Eulerian grid methods, and also some variants of Lagrangian smoothed particle hydrodynamics (SPH) methods.     

集主承力结构与大容量储箱支架于一体的卫星主承力筒结构研究

针对现代卫星结构的大型化、燃料储箱的大型化,提出了一种集主承力结构与大容量储箱支架一体化的卫星主承力筒结构形式,旨在降低卫星质心、提高基频;在满足储箱容积的前提下,又能满足主结构有效载荷往运载的力的传递作用.有限元数值计算表明,该结构形式能够满足卫星相关结构性能的要求,可以作为今后卫星结构设计的参考构型.     

Improving the process forming limit considering forming defects in the transitional region in local loading forming of Ti-alloy rib-web components

The isothermal local loading forming technology provides a feasible way to form Ti-alloy large-scale rib-web components in aerospace and aviation fields.However,the local load ing process forming limit is restricted by forming defects in the transitional region.In this work,the feasibility of controlling forming defects and improving the process forming limit by adjusting die parameters is explored through finite element (FE) simulation.It is found that the common cavum and folding defects in the transitional region are significantly influenced by the fillet radii of left rib and middle rib,respectively.The cavum and folding defects can be effectively controlled by increas ing the fillet radii of left rib and middle rib,respectively.The process forming limits considering forming defects in the transitional region are determined by the stepwise searching method under various die parameters.Moreover,the relationship between the process forming limit and die parameters is developed through the response surface methodology (RSM).The developed RSM models suggest that increasing the fillet radii of left and middle ribs is effective to improve the pro cess forming limit during local loading forming of rib-web components.The results will provide technical basis for the design of die parameters and the reduction amount,which is of great impor tance to control forming defects and improve the process forming limit in local loading forming of Ti-alloy large-scale rib-web components.     

应用快速多分类SVM的航空发动机故障诊断方法

提出了一种新的快速多分类SVM算法,用于解决大样本情况下航空发动机的多类故障诊断问题。首先,选用层次支持向量机(H-SVM)来实现多类分类,用各类数据中心代表该类数据,通过自组织特征映射神经网络(SOFM)进行聚类,把类中心之间距离较近的数据归为同一个子类进行训练,得到H-SVM层次结构。其次,在训练H-SVM中的二元分类器时,应用相对边界向量(RBV)代替全部训练样本,在保持分类精度几乎不变的条件下大幅度减少了训练样本数,使训练时间明显缩短;同时,由于支持向量的数量减小,分类时间也相应缩短。在分类数据混迭较为严重的情况下,新算法先剔除混迭的异类数据,再计算RBV,并且把与计算的RBV距离小于一定数值的样本都选择来训练SVM,保证了RBV的合理性,防止了关键数据的丢失,有效提高了分类精度。针对一个航空涡喷发动机5类复合故障的分类进行了实例仿真,总的故障分类正确率达到91.2%,二元SVM的训练时间最多只有原来的16.20%;当训练样本总数达到7500的大规模情况下,根据本算法,约减后的样本数量只有原来的3.05%。仿真结果表明,提出的算法有效、可靠,容易实现。     

基于互联网的导航定位增强信息大规模实时播发研究

在卫星导航系统中，可通过注入增强信息的方法提高导航定位精度、可靠性和完好性。导航定位增强信息一般由卫星播发，通过互联网播发导航定位增强信息是近期一个新的研究热点。本文综述了互联网播发技术的研究现状，提出了一个基于互联网的导航定位增强信息大规模实时播发系统模型，采用基于对等网络技术、具有自组织特性的分层混合结构覆盖网络，有效降低了系统构建和管理的复杂性。论文还分析了导航定位增强信息播发的实时性和安全性需求，并提出了解决思路。     

Numerical Simulations of the Warm-Hot Intergalactic Medium

In this paper we review the current predictions of numerical simulations for the origin and observability of the warm hot intergalactic medium (WHIM), the diffuse gas that contains up to 50 per cent of the baryons at z∼0. During structure formation, gravitational accretion shocks emerging from collapsing regions gradually heat the intergalactic medium (IGM) to temperatures in the range T∼10⁵–10⁷ K. The WHIM is predicted to radiate most of its energy in the ultraviolet (UV) and X-ray bands and to contribute a significant fraction of the soft X-ray background emission. While O vi and C iv absorption systems arising in the cooler fraction of the WHIM with T∼10⁵–10^5.5 K are seen in FUSE and Hubble Space Telescope observations, models agree that current X-ray telescopes such as Chandra and XMM-Newton do not have enough sensitivity to detect the hotter WHIM. However, future missions such as Constellation-X and XEUS might be able to detect both emission lines and absorption systems from highly ionised atoms such as O vii, O viii and Fe xvii.     

Generation of secondary waves due to intensive large-scale AGW traveling

By using data from GPS receivers we detected huge-amplitude solitary large-scale traveling acoustic-gravity waves (LS AGW) which manifested themselves as perturbations of total electron content (TEC) of duration of about 40 min. Originated in the auroral area after significant alterations of geomagnetic field intensity during geomagnetic storms on 29–30 October 2003, LS disturbances propagated with a velocity about 1000–1200 m/s and caused generation of secondary small-scale (SS) waves with time period of 2–10 min. Such SS structure followed the solitary intensive AGW at a distance more than 4000 km. However, we observed such phenomenon only within the territory with high values of “vertical” TEC and steep gradients of TEC. Apparently, these conditions are necessary for generation of SS waves due to propagation of LS AGW.     

大型航天器再入陨落时太阳翼气动力/热模拟分析

采用直接模拟蒙特卡洛（DSMC）方法对大型航天器离轨再入陨落过程中,其太阳翼帆板在稀薄过渡流域的气动力、气动热特性进行数值模拟,计算中采用流场直角与表面三角形非结构混合网格以及网格自适应技术处理这类复杂外形的流动模拟,考虑内能激发和化学反应来准确模拟气动加热,并基于MPI环境的并行算法解决计算量庞大的难题。通过计算分析太阳翼水平和垂直放置时在不同高度、不同攻角下的复杂流动特征,表明在90km以上高空,太阳翼垂直放置时,飞行器头部脱体激波与帆板脱体激波会产生更强烈、更复杂的激波/激波和激波/边界层的干扰,在气动力和气动热的双重作用下要比水平放置时的太阳翼更快地被撕裂并脱离目标航天器。