一种新的计算非稳态流动的自适应无网格方法

基于带权点填充布点方法,结合指定流场参数梯度的分布,提出了一种新的无网格自适应方法计算非稳态问题。该方法的自适应探测器 E 由节点的权重和参数梯度组成。使用自适应探测器识别出加密或者粗化的区域,形成加密空腔和粗化空腔,然后重新填充布点。新节点的权重由自适应探测器 E 结合该处的梯度大小通过预测-校正迭代算法计算得到。另外,由于参数梯度在激波附近波动范围比较大,所以新节点的权重存在最大值和最小值。首先对预先设置压强梯度的流场区域进行自适应布点,并与传统自适应布点结果进行对比,点云分布图显示所提自适应方法重新生成的点云结构疏密分布更加合理。进一步,将此自适应方法应用于 Riemann 问题和激波碰撞圆柱问题,计算结果表明该方法可以在节点数目较低的情况下显著提高运动激波的分辨率。在激波碰撞圆柱问题中,比较了使用自适应算法和非自适应算法得到相当的结果所使用时间,前者是后者的20.6%,因此该自适应算法在计算效率方面也具有较大的优势。     

Interplanetary shocks and geomagnetic activity during solar maximum (2000) and solar minimum (1995–1996)

Plasma and magnetic field parameter variations through fast forward interplanetary shocks were correlated with the peak geomagnetic activity index Dst in a period from 0 to 3 days after the shock, during solar maximum (2000) and solar minimum (1995–1996). Solar wind speed (V) and total magnetic field (B_t) were the parameters with higher correlations with peak Dst index. The correlation coefficients were higher during solar minimum (r² = 56% for V and 39% for B_t) than during solar maximum (r² = 15% for V and 12% for B_t). A statistical distribution of geomagnetic activity levels following interplanetary shocks was obtained. It was observed that during solar maximum, 36% and 28% of interplanetary shocks were followed by intense (Dst  −100 nT) and moderate (−50  Dst < −100 nT) geomagnetic activity, whereas during solar minimum 13% and 33% of the shocks were followed by intense and moderate geomagnetic activity. It can be concluded that the upstream/downstream variations of V and B_t through the shocks were the parameters better correlated with geomagnetic activity level, and during solar maximum a higher relative number of interplanetary shocks can be followed by intense geomagnetic activity than during solar minimum. One can extrapolate, for forecasting goals, that during a whole solar cycle a shock has a probability of around 50% to be followed by intense/moderate geomagnetic activity.     

多重激波的数值模拟研究

本文用一维混合粒子模拟Code研究了包括中间激波在内的多重激波.模拟了四种情形,可以分为两类:(1)由快激波和中间激波构成的两重激波,(2)快激波、中间激波和慢激波构成的三重激波.结果表明:多重激波是不稳定的,它趋向于发展成磁流体旋转间断和MHD波,左旋圆偏振波逐渐在上游区内发展起来.文章对导致多重激波不稳定性的可能原因进行了简单的讨论.     

蜂窝夹芯叠层板的低速冲击损伤分析

建立复合材料蜂窝夹芯叠层板（以下简称蜂窝板）低速冲击损伤模型,应用动态有限元分析程序估算蜂窝板低速冲击损伤的发生和扩展,该程序采用２０节点等参元和弹簧元分别模拟面板和促使闪芯,该模型建立在面板的初始损伤准则（蔡－胡强度准则）和损伤扩展准则（Ｆ．Ｋ．Ｃｈａｎｇ的冲击分层损伤判据）以及本文提出的蜂窝夹芯的简化损伤准则的基础上,并进行了低速冲击损伤实验以验证模拟计算结果,比较表明预测结果与实验数据吻合较     

Reverse shock acceleration of electrons and protons at mid-heliolatitudes from 5.3-3.8 AU

We examine the intensity, anisotropy and energy spectrum of 480–966 keV protons and 38–315 keV electrons observed by the HI-SCALE instrument on Ulysses associated with Corotating Interaction Regions (CIR) from mid-1992 to early 1994. The particle events are most clearly ordered by the reverse shocks bounding the CIRs. The bulk of the ion fluxes appear either straddling, or with their maximum intensity following, the reverse shock. The electron intensities rise sharply to their maximum upon the passage of the reverse shock, and are delayed with respect to the protons. We believe that following acceleration at the reverse shock the electrons re-enter the inner heliosphere and mirror, to return to the reverse shock for repeated acceleration. This process is more effective for electrons (vc/2) than for ions, and also favours the higher velocity electrons, which accounts for the observed spectral hardening with latitude.     

Perpendicular Shock Reformation and Ion Acceleration

Kinetic simulations of supercritical, quasi-perpendicular shocks yield time-varying solutions that cyclically reform on proton spatio-temporal scales. Whether a shock solution is stationary or reforming depends upon the plasma parameters which, for SNR shocks and the heliospheric termination shock, are ill defined but believed to be within this time-dependent regime. We first review the time-dependent solutions and the acceleration processes of the ions for a proton–electron plasma. We then present recent results for a three-component plasma: background protons, electrons and a second ion population appropriate for SNR (heavy ions) or the termination shock (pickup protons). This ion acceleration generates a suprathermal “injection” population – a seed population for subsequent acceleration at the shock, which may in turn generate ions at cosmic ray energies.     

Correlation between sunspots and interplanetary shocks measured by ACE during 1998–2014 and some estimations for the 22nd solar cycle and the years between 2015 and 2018 with artificial neural network using the Cavus 2013 model

The Advanced Composition Explorer (ACE) spacecraft has measured 235 solar-based interplanetary (IP) shock waves between the years of 1998–2014. These were composed of 203 fast forward (FF), 6 slow forward (SF), 21 fast reverse (FR) and 5 slow reverse (SR) type shocks. These data can be obtained from the Interplanetary Shock Database of Harvard-Smithsonian Centre for Astrophysics. The Solar Section of American Association of Variable Star Observers (AAVSO) is an organization that counts the number of the sunspots. The effects of interplanetary shock waves on some physical parameters can be computed using a hydrodynamical model. There should be some correlations between these effects and the sunspot variations. The major objective of this paper is twofold. The first one is to search these correlations with sunspots given in the database of AAVSO. As expected, high correlations between physical parameters and sunspots have been obtained and these are presented in tables below. The second objective is to make an estimation of these parameters for the 22nd solar cycle and the years between 2015 and 2018 using an artificial neural network. Predictions have been made for these years where no shock data is present using artificial intelligence. The correlations were observed to increase further when these prediction results were included.     

Exploring the global shock scenario at multiple points between sun and earth: The solar transients launched on January 1 and September 23, 1978

We revisit the transient interplanetary events of January 1 and September 23, 1978. Using in-situ and remote sensing observations at locations widely separated in longitudes and distances from the Sun, we infer that in both cases the overall shock surface had a very fast “nose” region with speeds >900 and >1500 km⁻¹ in the January and September events, respectively, and much slower flank speeds (∼600 km⁻¹ or less), suggesting a shock surface with a strong speed gradient with heliospheric longitude. The shock-nose regions are thus likely efficient acceleration sites of MeV ions, even at 1 AU from the Sun. Our 3D magnetohydrodynamics modeling suggests that a 24° × 24° localized disturbance at 18 solar radii injecting momentum 100 times the background solar wind input over 1 h can produce a disturbance in semi-quantitative agreement with the observed shock arrival time, plasma density and velocity time series in the January 1978 event.     

烧蚀外形三维粘性流场数值模拟

本文通过求解层流Navier-Stokes方程,数值模拟了三维奶头型烧蚀外形粘性流场。差分格式为Yee和Harten的迎风隐式TVD格式,在空间方向具有二阶精度。计算得到了高质量的激波和合理的流场结构。物面压力分布与实验结果进行比较,符合较好。     

曲梁弹性波的传播

用特征线法求出了脉冲载荷作用下的控制曲梁运动的Ｍｏｒｌｅｙ方程的数值解，并用Ｐｌａｓｓ的直梁结果验证了曲率趋于零的极限情形，应用性地研究了曲梁中部受冲击载荷作用的弹性波传播问题，计算结果表明：该数值计算方法简便易行、效率高、有良好的收敛性和稳定性。