某小型发动机环形回流燃烧室流场的数值计算

采用数值模拟方法对某小型发动机回流燃烧室流场进行了计算和分析,用双方程k-ε模型描述紊流特性,用二步化学反应模型模拟化学反应,并对复杂的边界条件进行了特殊处理。计算结果表明火焰筒主燃区形成了强烈的单涡回流,沿圆周方向主燃区速度场比较相似;在油雾场和速度场之间有较好的匹配,燃烧室有较好的性能。      

共轴式双旋翼悬停流场的水洞PIV测量

采用粒子图像测速(PIV)技术,对共轴式双旋翼在悬停状态下的流场进行水洞实验,测量得到旋翼流场的涡量和速度分布,桨尖涡的结构和脱落轨迹等直观整体的图像,研究了共轴式双旋翼悬停流场的气动干扰特性.为了比较,对单旋翼也进行测量.实验结果为直升机的气动计算和合理设计提供了可靠的实验依据.      

高超声速钝锥体等离子体流场数值模拟

以小钝锥体为对象建立二维几何模型,利用COMSOL Multiphysics软件对等离子体流场控制方程组进行求解,对高超声速气流流过模型所产生的等离子体流场进行数值模拟.仿真得到了在模型头部激波、尾部膨胀波和尾后激波的共同作用下,考虑烧蚀反应时流场的速度、温度、压强和等离子体电子数密度分布,重点分析了钝锥体模型等离子体包覆层和尾后电子分布的特征和成因.可以为高超声速飞行器的探测和控制提供重要的借鉴和参考.     

正弯涡轮叶栅内旋涡结构的数值模拟

对某型涡轮正弯及直叶栅流场进行了三维粘性求解。给出了马蹄涡及通道涡的详细演化过程。通过对弯直叶栅两类流场拓扑结构上的差异分析,指出与直叶栅相比采用合适的弯角后正弯叶栅有利于形成稳定的通道涡,并且在相当大的轴向弦长范围内保持着这种稳定的涡结构。并将其对损失的影响进行了分析     

GH909电子束焊接温度场的有限元分析

采用MARC有限元分析软件对GH909电子束焊接热过程进行了数值模拟.针对电子束焊不同于普通电弧焊的特殊加热方式,提出了小孔内壁受热的能量输入模式.与工件表面高斯分布的能量输入模式相比,该模式考虑了小孔形成对能量吸收的影响,因此所得到的模拟结果更好地反映了电子束焊缝的形状特点.     

Analysis of a long-duration AR throughout five solar rotations: Magnetic properties and ejective events

Coronal mass ejections (CMEs), which are among the most magnificent solar eruptions, are a major driver of space weather and can thus affect diverse human technologies. Different processes have been proposed to explain the initiation and release of CMEs from solar active regions (ARs), without reaching consensus on which is the predominant scenario, and thus rendering impossible to accurately predict when a CME is going to erupt from a given AR. To investigate AR magnetic properties that favor CMEs production, we employ multi-spacecraft data to analyze a long duration AR (NOAA 11089, 11100, 11106, 11112 and 11121) throughout its complete lifetime, spanning five Carrington rotations from July to November 2010. We use data from the Solar Dynamics Observatory to study the evolution of the AR magnetic properties during the five near-side passages, and a proxy to follow the magnetic flux changes when no magnetograms are available, i.e. during far-side transits. The ejectivity is studied by characterizing the angular widths, speeds and masses of 108 CMEs that we associated to the AR, when examining a 124-day period. Such an ejectivity tracking was possible thanks to the multi-viewpoint images provided by the Solar-Terrestrial Relations Observatory and Solar and Heliospheric Observatory in a quasi-quadrature configuration. We also inspected the X-ray flares registered by the GOES satellite and found 162 to be associated to the AR under study. Given the substantial number of ejections studied, we use a statistical approach instead of a single-event analysis. We found three well defined periods of very high CMEs activity and two periods with no mass ejections that are preceded or accompanied by characteristic changes in the AR magnetic flux, free magnetic energy and/or presence of electric currents. Our large sample of CMEs and long term study of a single AR, provide further evidence relating AR magnetic activity to CME and Flare production.     

Topological and statistical properties of nonlinear force-free fields

We use our semi-analytic solution of the nonlinear force-free field equation to construct three-dimensional magnetic fields that are applicable to the solar corona and study their statistical properties for estimating the degree of braiding exhibited by these fields. We present a new formula for calculating the winding number and compare it with the formula for the crossing number. The comparison is shown for a toy model of two helices and for realistic cases of nonlinear force-free fields; conceptually the formulae are nearly the same but the resulting distributions calculated for a given topology can be different. We also calculate linkages, which are useful topological quantities that are independent measures of the contribution of magnetic braiding to the total free energy and relative helicity of the field. Finally, we derive new analytical bounds for the free energy and relative helicity for the field configurations in terms of the linking number. These bounds will be of utility in estimating the braided energy available for nano-flares or for eruptions.     

Neutral atmosphere and crustal magnetization as factors determining differences in plasma convection and magnetic fields distribution in the ionospheres of Mars and Venus

The pattern of the magnetic field/plasma convection can be, to some extent, recovered from the magnetic field measurements by employing either theoretical or numerical models. We use the MAG/ER day-time measurements of the magnetic field at the altitudes from 90 to 180 km during the elliptical orbits of MGS. Analysis of the altitude variation of the characteristics of the large-scale magnetic fields, which were measured some distance away from strong crustal magnetic anomalies, is summarized. The low density of the Martian atmosphere together with the crustal magnetization result in critical differences in plasma convection which are followed by remarkable differences of the magnetic field features within the ionosphere of Venus and Mars (even in its northern hemisphere where the crustal magnetization is, on the average, low) and distribution of currents.     

(70~100)MeV准单能中子参考辐射场设计

国内基于串列加速器建立了144keV~15MeV的单能中子参考辐射场，解决了20MeV以下能区中子探测器注量、剂量等参数的量值溯源，但尚未建立20MeV以上能区准单能中子参考辐射场。随着航天空间中子探测任务的需要以及地面高能质子加速器的发展，20MeV以上能区准单能中子参考辐射场需求越来越突出。发展20MeV以上能区高能中子参考辐射场对于满足国防需求、推动中子计量学科发展具有重要意义。     

Three-dimensional magnetic reconnection regimes: A review

The magnetic field in many astrophysical plasmas – such as the solar corona and Earth’s magnetosphere – has been shown to have a highly complex, three-dimensional structure. Recent advances in theory and computational simulations have shown that reconnection in these fields also has a three-dimensional nature, in contrast to the widely used two-dimensional (or 2.5-dimensional) models. Here we discuss the underlying theory of three-dimensional magnetic reconnection. We also review a selection of new models that illustrate the current state of the art, as well as highlighting the complexity of energy release processes mediated by reconnection in complicated three-dimensional magnetic fields.