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.     

On the Origin of the Strong Intermittent Nature of Interplanetary Magnetic Field

We briefly discuss the strong intermittent nature of the interplanetary magnetic field, observing that similarity between its statistical properties and the passive scalar ones exists, and may arise from different dynamical mechanisms.     

Shocks: Commonalities in Solar-Terrestrial Chains

Shocks are found throughout the heliosphere, wherever supersonic (or super-magnetosonic) flows encounter obstacles or other, slowly moving, media. Although some of the physical parameters are in different regimes, all shocks heat and decelerate the media incident upon them. Most shocks must propagate in a collisionless plasma, thereby adding importance to the particle interactions with the electromagnetic fields, and enabling some particles to be accelerated to high energies. This paper explores the commonalities, and differences, in shocks throughout the heliosphere, and concentrates on the role of shock microstructure in effecting the shock transition and in governing the resulting energy partition amongst the constituent species. Shocks play a significant role in the solar-terrestrial chain.     

X射线脉冲星导航在行星际轨道上的应用

X射线脉冲星导航技术被认为是新一代导航技术,非常适合于行星际探测.深入分析了利用搜索空间方法求解飞行器真实位置和估计位置相位差的脉冲整周期模糊数,解决了相位导航方法存在的周期模糊数问题.利用轨道动力学模型估计飞行器的位置,并以真实位置和估计位置上的脉冲相位之差作为反馈进行偏差校正.仿真表明,X射线脉冲星导航方法在行星际轨道上是可行和高效的.     

Working Group 3 Report: Coronal Hole Boundaries and Interactions with Adjacent Regions

Summarized below are the discussions of working group 3 on "Coronal hole boundaries and interactions with adjacent regions" which took place at the 7th SOHO workshop in Northeast Harbor, Maine, USA, 28 September to 1 October 1998. A number of recent observational and theoretical results were presented during the discussions to shed light on different aspects of coronal hole boundaries. The working group also included presentations on streamers and coronal holes to emphasis the difference between the plasma properties in these regions, and to serve as guidelines for the definition of the boundaries. Observations, particularly white light observations, show that multiple streamers are present close to the solar limb at all times. At some distance from the sun, typically below 2 R, these streamers merge into a relatively narrow sheet as seen, for example, in LASCO and UVCS images. The presence of multiple current sheets in interplanetary space was also briefly addressed. Coronal hole boundaries were defined as the abrupt transition from the bright appearing plasma sheet to the dark coronal hole regions. Observations in the inner corona seem to indicate a transition of typically 10 to 20 degrees, whereas observations in interplanetary space, carried out from Ulysses, show on one hand an even faster transition of less than 2 degrees which is in agreement with earlier Helios results. On the other hand, these observations also show that the transition happens on different scales, some of which are significantly larger. The slow solar wind is connected to the streamer belt/plasma sheet, even though the discussions were still not conclusive on the point where exactly the slow solar wind originates. Considered the high variability of plasma characteristics in slow wind streams, it seems most likely that several types of coronal regions produce slow solar wind, such as streamer stalks, streamer legs and open field regions between active regions, and maybe even regions just inside of the coronal holes. Observational and theoretical studies presented during the discussions show evidence that each of these regions may indeed contribute to the solar slow wind. This revised version was published online in June 2006 with corrections to the Cover Date.     

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。     

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.     

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.     

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.     

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