The characteristics of sharp (small-scale) boundaries of solar wind plasma and magnetic field structures

We investigate properties of large (>20%) and sharp (<10 min) solar wind ion flux changes using INTERBALL-1 and WIND plasma and magnetic field measurements from 1996 to 1999. These ion flux changes are the boundaries of small-scale and middle-scale solar wind structures. We describe the behavior of the solar wind velocity, temperature and interplanetary magnetic field (IMF) during these sudden flux changes. Many of the largest ion flux changes occur during periods when the solar wind velocity is nearly constant, so these are mainly plasma density changes. The IMF magnitude and direction changes at these events can be either large or small. For about 55% of the ion flux changes, the sum of the thermal and magnetic pressure are in balance across the boundary. In many of the other cases, the thermal pressure change is significantly more than the magnetic pressure change. We also attempted to classify the types of discontinuities observed.     

Sharp boundaries of solar wind plasma structures and their relationship to solar wind turbulence

Sharp (<10 min) and large (>20%) solar wind ion flux changes are common phenomena in turbulent solar wind plasma. These changes are the boundaries of small- and middle-scale solar wind plasma structures which can have a significant influence on Earth’s magnetosphere. These solar wind ion flux changes are typically accompanied by only a small change in the bulk solar wind velocity, hence, the flux changes are driven mainly by plasma density variations. We show that these events occur more frequently in high-density solar wind. A characteristic of solar wind turbulence, intermittency, is determined for time periods with and without these flux changes. The probability distribution functions (PDF) of solar wind ion flux variations for different time scales are calculated for each of these periods and compared. For large time scales, the PDFs are Gaussian for both data sets. For small time scales, the PDFs from both data set are more flat than Gaussian, but the degree of flatness is much larger for the data near the sharp flux change boundaries.     

强磁场扰动对宇宙线调制的统计研究

对1978─1982太阳活动高年时发生的激波、强磁场扰动及激波与强磁场扰动共存这三类事件引起的宇宙线变化进行了统计研究,得到如下结果:(1)激波与强磁场扰动共存时引起的宇宙线强度下降最为显着;只有激波或强磁场扰动时,宇宙线的强度变化相对较小;(2)标志速度间断的激波是产生宇宙线Forbush下降的重要因素;(3)速度间断在强磁场扰动对宇宙线的调制中可能起一个触发的作用。      

Global Hybrid Simulation of Magnetic Reconnection in the Magnetosheath

A three-dimensional (3-D) global hybrid simulation is carried out for the generation and structure of magnetic reconnection in the magnetosheath due to interaction of an interplanetary Tangential Discontinuity (TD) with the bow shock and magnetosphere. Runs are performed for solar wind TDs possessing different initial half-widths. As the TD propagates through the bow shock toward the magnetopause, it is greatly narrowed by a two-step compression processes, a "shock compression' followed by a subsequent ``convective compression'. In cases with a relatively thin solar wind TD, 3-D patchy reconnection is initiated in the transmitted TD, forming magnetosheath flux ropes. Multiple components of ion particles are present in the velocity distribution in the magnetosheath merging, accompanied by ion heating. For cases with a relatively wide initial TD, a dominant single X-line appears in the subsolar magnetosheath after the transmitted TD is narrowed. A shock analysis is performed for the detailed structure of magnetic reconnection in the magnetosheath. Rotational Discontinuity (RD)/Time-Dependent Intermediate Shock (TDIS) are found to dominate the reconnection layer, which and some weak slow shocks are responsible for the ion heating and acceleration.      

Possible physical properties of the flow in the vicinity of the heliopause

An interface between the fully ionized hydrogen plasma of the solar wind (SW) and the partially ionized hydrogen gas flow of the local interstellar medium (LISM) is formed as a region where there is a strong interaction between these two flows. The interface is bounded by the solar wind termination shock (TS) and the LISM bow shock (BS) and is separated on two regions by the heliopause (HP) separating the solar wind and charged component of the LISM (plasma component below). The BS is formed due to the deceleration of the supersonic LISM flow relative to the solar system. Regions of the interface between the TS and HP and between the HP and BS were in literature named as the inner and outer heliosheaths, respectively. An investigation of the structure and physical properties of the heliosheath is at present especially interested due to the fact that Voyager-1 and Voyager-2 have crossed the TS in December 2004 (Burlaga, L.F., Ness, N.F., Acuna, M.Y., et al. Crossing the termination shock into the the heliosheath. Magnetic fields. Science 309, 2027–2029, 2005; Fisk, L.A. Journey into the unknown beyond. Science 309, 2016–2017, 2005; Decker, R.B., Krimigis, S.M., Roelof, E.C., et al. Voyager 1 in the foreshock, termination shock and heliosheath. Science 309, 2020–2024, 2005; Stone, E.C., Cummings, A.C., McDonald, F.B., et al. Voyager 1 explores the termination shock region and the heliosheath beyond. Science 309, 2017–2020, 2005) and in September 2007 (Jokipii, J.R. A shock for Voyager 2. Nature 454, 38–39, 2008; Gurnett, D.A., Kurth, W.S. Intense plasma waves at and near the solar wind termination shock. Nature 454, 78–80, 2008. doi: 10.1038/nature07023; Wang, L., Lin, R.P., Larson, D.E., Luhmann, J.G. Domination of heliosheath pressure by shock-accelerated pickup ions from observations of neutral atoms. Nature 454, 81–83, 2008. doi: 10.1038/nature07068.14; Burlaga, L.F., Ness, N.F., Acuna, M.H., et al. Magnetic fields at the solar wind termination shock. Nature 454, 75–77, 2008. doi: 10.1038/nature07029; Richardson, J.D., Kasper, J.C., Wang, C., et al. Cool heliosheath plasma and deceleration of the upstream solar wind at the termination shock. Nature 454, 63–66, 2008. doi: 10.1038/nature07024; Stone, E.C., Cummings, A.C., McDonald, F.B., et al. An asymmetric solar wind termination shock. Nature 454, 71–74, 2008. doi: 10.1038/nature07022; Decker, R.B., Krimigis, S.M., Roelof, E.C., et al. Mediation of the solar wind termination shock by non-thermal ions. Nature 454, 67–70, 2008. doi: 10.1038/nature 07030), respectively, and entered to the inner heliosheath.     

IMPLICIT REPRESENTATION FOR THE MODELLING OF HYBRID DYNAMIC SYSTEMS

Differentmodels are proposed for the study ofhybrid systems that are composed of interactingcontinuous and discrete parts as,for instance,inRef.[1 ].Generally,the discrete part is modelledby an automation,and the continuous part by dif-ferent sets of state equations.Jump functions canbe added to represent the discontinuities.But noindication is given about the relations between thedifferent models and the jump functions.　　This paper isconcerned with the modelling forphysical systems with sw…     

脊波导接头的模匹配分析

文章给出了严密的脊波导本征函数的表达式,并运用驻波法推导了完整的脊波导的特征方程;采用模匹配法分析了矩形-脊波导不连续性的广义S矩阵,数值仿真与HFSS仿真结果一致。     

基于IDS的铝合金预腐蚀疲劳寿命研究

 模拟飞机服役环境,对航空LY12铝合金试验件做了腐蚀试验,然后通过疲劳试验得到LY12铝合金新试验件和预腐蚀试验件的疲劳寿命数据。分析了腐蚀对航空LY12铝合金的影响。通过观测断面腐蚀坑的尺寸,基于初始不连续状态（IDS）建立了把腐蚀坑看做表面裂纹的几种模型,并对几种裂纹模型的疲劳寿命计算结果和实际试验结果进行了对比分析。结果表明：直接把腐蚀坑看做表面裂纹是不合理的,考虑材料初始不连续状态所建立的表面裂纹模型计算结果和试验结果比较吻合;随着腐蚀坑的增大,裂纹模型2更为合理。所以,很难用一个合适的裂纹模型来描述腐蚀坑,只有把腐蚀坑分组才有可能得出更精确的描述。     

剥蚀对飞机机翼上蒙皮疲劳寿命的影响分析

剥蚀是影响老龄飞机机翼结构完整性的重要因素之一.文中基于材料的初始不连续状态(initial discontinuity state, IDS),建立了评估剥蚀对机翼上蒙皮疲劳寿命影响的模型,然后利用AFGROW计算了在以压应力为主导的等幅载荷谱作用下,机翼蒙皮针对不同腐蚀损伤程度时的疲劳寿命.还研究了多腐蚀损伤对机翼蒙皮疲劳寿命的影响,结果表明,相对于单腐蚀损伤,多腐蚀损伤大大降低结构的疲劳寿命,但其对剥蚀程度不敏感.与试验结果比较表明,该模型预测结果精确,方法可靠.