S波自旋单态底夸克偶素衰变到粲夸克对

对S波自旋单态底夸克偶素衰变到粲夸克对进行了研究,同时还研究了S波自旋单态和自旋三重态底夸克偶素衰变到D介子对。利用BaBar实验组测量得到的自旋三重态底夸克偶素衰变到D介子分支比的数据,发现自旋三重态底夸克偶素的色八重态矩阵元远小于理论预言,理论预言要比实验上限大20倍以上;得到S波自旋单态底夸克偶素衰变到粲夸克对的分支比的理论预言,可以进行实验测量从而研究色八重态矩阵元;得到S波自旋单态底夸克偶素衰变到D介子对的分支比的理论预言,与其他理论预言差异较大。这些预言可以通过BelleⅡ的实验进行验证,从而得到更多强子化的信息。      

激波过弯道绕山坡对三维物体的冲击效应研究

采用全息干涉技术在高速流态试验装置 (激波管 )上研究了激波过弯道绕山坡到达三维物体的整个过程的流场 ,还采用传感器压力测量技术对三维物体表面的压力分布进行了定量测量。结果表明 ,激波对三维物体与山坡的接合部、物体背风面及其拐角位置的影响是最大的 ;对于研究爆炸冲击波在复杂地形下对建筑物的冲击载荷有重要意义。     

地-月L2点中继星月球近旁转移轨道设计

位于地月L2点周期轨道的中继星将首次为"嫦娥4号"月球背面着陆探测任务提供通信中继服务。中继星转移轨道设计是中继任务实施的关键环节。针对中继星转移轨道存在转移时间、近月点高度和halo轨道振幅等约束条件,系统研究了基于月球近旁的地月L2点转移轨道设计方法。首先基于限制性三体模型,分析了halo轨道族与着陆点可见性关系;然后将月球近旁转移轨道分为地月直接转移段和地月动平衡点附近周期轨道拟流形入轨转移段,采用带有状态约束的微分修正算法对这两段轨道进行拼接,得到了从地球附近至目标轨道族的月球近旁转移轨道;最后,针对南族halo轨道分析了halo轨道振幅和月球飞越高度对转移轨道设计的影响,以及转移轨道的入轨相位分布。仿真结果表明:月球近旁转移轨道设计方案具备工程上的可行性与优越性。该方案可以为实际工程任务和应用提供参考。     

ZrB2 及其复合陶瓷的高温抗氧化性能

综述了ZrB_2及其复合陶瓷的高温氧化行为,认为ZrB_2陶瓷是一种优异的高温结构材料,其氧化失效是由于氧化产物B_2O_3保护层挥发失效而导致的;二元陶瓷ZrB_2-SiC由于SiC的加入,高温抗氧化性能大大提高,并对其在不同温度下的氧化物结构进行了阐述。在此基础上提出了进一步提高ZrB_2-SiC陶瓷抗氧化性能和服役温度的方法,并以添加TaC和LaB_6形成三元复相陶瓷为例进行了说明。     

浅析大飞机数字化设计与制造技术

大飞机工程是一个国家具有战略性的高技术产业链,而数字化技术在大飞机设计制造过程中的应用有效推进了大飞机的设计制造进程.论述了大飞机数字化技术的几个典型特征,并从设计制造的9个方面浅析了数字化技术在大飞机设计制造中的应用,涵盖了大飞机设计制造的大多数领域.展望未来数字化技术将会越来越深入地融入到大飞机设计与制造的每个角落.     

逆向工程的关键技术及其研究

综述了逆向工程中实物数字化技术、测量数据的预处理、曲面重建技术、重构曲面的评价和检验等关键技术的发展现状和存在的问题,并对今后的发展方向进行了讨论。     

3D打印骨架增强石蜡燃料燃烧机理实验研究

针对固-液混合火箭发动机中石蜡基固体燃料机械性能差的问题,使用3D打印聚合物骨架镶嵌石蜡的方法增强了石蜡基燃料的结构强度,分析了骨架增强石蜡燃料在直/旋流喷注下的燃烧机理。通过对七种骨架材料进行SEM扫描、力学、热力学分析和纯氧条件下的燃烧试验,获得了不同骨架材料的微观表面结构、机械性能、热分解性能以及在纯氧环境下的燃烧性能;使用直/旋流固-气掺混燃烧试验系统,开展了螺旋型和六角型骨架增强石蜡燃料的燃烧试验,并与ABS固体燃料进行了对比。结果显示,在多种骨架材料中,ABS材料加工性能、机械性能及热分解性能良好;燃烧过程中,骨架增强石蜡燃料结构稳定性良好,石蜡液滴主要出现在石蜡-骨架交界处;旋流喷注和螺旋型骨架可促进石蜡液滴的夹带现象;在直流喷注工况中,骨架的凹槽结构增加了燃料与氧化剂的接触面积,尾部骨架结构具有稳焰作用,可促进后燃烧室的掺混燃烧;石蜡燃料和骨架燃速差异较大,发动机内弹道性能可能受此影响。     

Comparison of ionospheric F2 peak parameters foF2 and hmF2 with IRI2001 at Hainan

Monthly median values of foF2, hmF2 and M(3000)F2 parameters, with quarter-hourly time interval resolution for the diurnal variation, obtained with DPS4 digisonde at Hainan (19.5°N, 109.1°E; Geomagnetic coordinates: 178.95°E, 8.1°N) are used to investigate the low-latitude ionospheric variations and comparisons with the International Reference Ionosphere (IRI) model predictions. The data used for the present study covers the period from February 2002 to April 2007, which is characterized by a wide range of solar activity, ranging from high solar activity (2002) to low solar activity (2007). The results show that (1) Generally, IRI predictions follow well the diurnal and seasonal variation patterns of the experimental values of foF2, especially in the summer of 2002. However, there are systematic deviation between experimental values and IRI predictions with either CCIR or URSI coefficients. Generally IRI model greatly underestimate the values of foF2 from about noon to sunrise of next day, especially in the afternoon, and slightly overestimate them from sunrise to about noon. It seems that there are bigger deviations between IRI Model predictions and the experimental observations for the moderate solar activity. (2) Generally the IRI-predicted hmF2 values using CCIR M(3000)F2 option shows a poor agreement with the experimental results, but there is a relatively good agreement in summer at low solar activity. The deviation between the IRI-predicted hmF2 using CCIR M(3000)F2 and observed hmF2 is bigger from noon to sunset and around sunrise especially at high solar activity. The occurrence time of hmF2 peak (about 1200 LT) of the IRI model predictions is earlier than that of observations (around 1500 LT). The agreement between the IRI hmF2 obtained with the measured M(3000)F2 and the observed hmF2 is very good except that IRI overestimates slightly hmF2 in the daytime in summer at high solar activity and underestimates it in the nighttime with lower values near sunrise at low solar activity.     

Mapping lunar surface chemistry: New prospects with the Chandrayaan-2 Large Area Soft X-ray Spectrometer (CLASS)

Surface chemistry of airless bodies in the solar system can be derived from remote X-ray spectral measurements from an orbiting spacecraft. X-rays from planetary surfaces are excited primarily by solar X-rays. Several experiments in the past have used this technique of X-ray fluorescence for deriving abundances of the major rock forming elements. The Chandrayaan-2 orbiter carries an X-ray fluorescence experiment named CLASS that is designed based on results from its predecessor C1XS flown on Chandrayaan-1. We discuss the new aspects of lunar science that can be potentially achieved with CLASS.     

A broad climatology of very high latitude substorms

Magnetic data from a newly commissioned Indian Antarctic station Bharati (corrected geomagnetic (CGM) coordinates 74.7°S, 97.2°E) and closely-spaced IMAGE chain observatories (∼100° magnetic meridian in Northern hemisphere) has been analyzed to study the climatology of substorms which were localized poleward of the standard auroral oval. We considered four austral summers (year 2007–2010) when data from Bharati was available. Several very high latitude substorms were observed in this duration when the solar activity remained unexpectedly low for a long time. Various features of very high latitude substorms, e.g., local time dependence, interplanetary state, hemispherical asymmetry and their nightside low latitude signatures are examined. Events studied here, suggested the following properties of substorms occurring at very high latitudes: (1) maximum occurrence was observed near magnetic midnight (21:00–02:00 MLT). (2) In contradiction to earlier reports, many substorms were observed even during negative IMF Bz condition. In addition, majority of substorms occurred during low or moderate solar wind streams. (3) Magnetic signatures were often pronounced in the winter hemisphere. (4) Even if widely used standard AE indices fail to monitor very high latitude substorms, their low latitude signatures are often evident.