Influence of the Interstellar Magnetic Field and Neutrals on the Shape of the Outer Heliosphere

Formed as a result of the solar wind (SW) interaction with the circum-heliospheric interstellar medium (CHISM), the outer heliosphere is generically three-dimensional because of the SW asphericity and the action of the interstellar and interplanetary magnetic fields (ISMF and IMF). In this paper we show that charge exchange between neutral and charged components of the SW–CHISM plasmas plays a dominant role not only in determining the geometrical size of the heliosphere, but also in the modulation of magnetic-field-induced asymmetries. More specifically, charge exchange between SW and CHISM protons and primary neutrals of interstellar origin always acts to decrease the asymmetry of the termination shock and the heliopause, which can otherwise be very large. This is particularly pronounced because the ionization ratio of the CHISM plasma is rather low. To investigate the deflection of the CHISM neutral hydrogen flow in the inner heliosphere from its original orientation in the unperturbed CHISM, we create two-dimensional neutral H velocity distributions in the inner heliosphere within a 45-degree circular conical surface with the apex at the Sun and the axis parallel to the interstellar flow vector. It is shown that the distribution of deflections is very anisotropic, that is, the most probable orientation of the H-atom velocity differs from its average direction. We show that the average deflection of the H-atom flow, for reasonable ISMF strengths, occurs mostly in the plane formed by the ISMF and CHISM velocity vectors at infinity. The possibility that the ISMF orientation may influence the 2–3 kHz radio emission, which is believed to originate in the outer heliosheath, is discussed.     

Temporal and Spatial Variation of the Ion Composition in the Ring Current

A global view of the ring current ions is presented using data acquired by the instrument MICS onboard the CRRES satellite during solar maximum. The variations of differential intensities, energy spectra, radial profile of the energetic particles and the origin of the magnetic local time (MLT) asymmetry of the ring current have been investigated in detail. O⁺ ions are an important contributor to the storm time ring current. Its abundance in terms of number density increases with increasing geomagnetic activity as well as its energy density. However, a saturation value for the energy density of O⁺ ions has been found. The low-energy H⁺ ions show a dramatic intensification and a rapid decay. However, its density ratio during the storm maximum is almost constant. On the other hand, high-energy H⁺ ions first exhibit a flux decrease followed by a delayed increase. Its density ratio shows an anti-correlation with the storm intensity. Both the positions of the maximum flux of O⁺ and He⁺ depend on storm activity: they move to lower altitudes in the early stage of a storm and move back to higher L-values during the recovery phase. Whereas the position of H⁺ and He⁺⁺ show almost no dependence on the Dst index. The energy density distributions in radial distance and magnetic local time show drastic differences for different ion species. It demonstrates that the ring current asymmetry mainly comes from oxygen and helium ions, but not from protons. The outward motion of O⁺ around local noon may have some implications for oxygen bursts in the magnetosheath during IMF Bz negative conditions as observed by GEOTAIL.     

圆柱容器液体晃动问题的数值计算

本文将二维VOF方法推广到三维情形,研究了圆柱容器遭受水平强迫振荡时的液体晃动问题。在数值模型中,采用了改进的施主与受主单元体方法计算流体在单元体之间的交换。同时对处理任意容器边界的部分单元体方法进行了改进,使之满足边界面上的速度边界条件。应用改进后的VOF方法得到的结果与试验结果符合较好,能够成功地数模出由于动力不稳定性引起的圆柱容器遭受纵向水平振荡时液体表面的旋转运动响应。     

Plasma-induced sputtering of an atmosphere

Magnetospheric ions, solar wind ions, and locally produced pick-up ions can impact the atmospheres of objects in the solar system, transferring energy by collisions with atmospheric atoms and molecules. This can result in an expansion of the atmospheric corona with a fraction of the energetic atoms or molecules being lost (sputtered) from the atmosphere. The expanded corona presents a larger target to the incident plasma, which in turn enhances pick-up ion formation and collisional ejection. In this manner a significant flux of atoms or molecules can be lost from an atmosphere, affecting its long-term evolution. This has been shown to be an important process for the dynamics and evolution of the atmosphere of lo, which is bombarded by the Jovian magnetospheric plasma, and for loss of atmosphere from Titan. Sputtering by pick-up ion bombardment has been shown to remove material from the atmosphere of Mars affecting the observed isotope ratios, and energetic O⁺ precipitation affects the Earth's thermosphere. The physics of ion bombardment of a gas which leads to atmospheric sputtering is described here. Analytic expressions derived from transport equations are shown to be useful for estimating the sputtering rate. These are compared to results from transport and Monte-Carlo calculations.     

一种全自动的检测方法用于SAR-ATI的GMTI

针对星载SAR-ATI处理的中间结果,提出了一种称为"两步-类高斯拟合"完全自适应的检测方法。该方法可以完全自动地实现杂波和噪声中的运动目标检测,避免了传统方法作联合高斯数据的假定,无须推导SAR-ATI干涉图的理论概率密度函数。此外,该方法还可以大大降低系统的虚警概率并用仿真研究了最小可检测速度。     

三维可压缩非定常流的壁面分离判据及其分离线附近的流动形态

通过引入依赖于密度的物面法向速度变换wr=-1/ρh1h2∫ozh1h2(e)ρ/(e)tdz,描述物理速度空间(ua,va,wa=u,v,w+wr)具有无滑移壁面条件的三维可压缩非定常连续方程可转换成变换速度空间(u,v,w)内具有无滑移条件定常连续方程.因此,采用定常壁面分离的分析方法和结论,再通过变换和研究wr的贡献,给出了三维可压缩非定常壁面分离的判则以及分离线附近的流动形态.研究指出,二维和三维情况下,都出现伴有壁外附着的壁面分离情况.数值模拟证实了理论和结论.     

直射式喷嘴喷雾特性的实验研究

用二维激光测速测粒仪,对直射式喷嘴在横向气流中所形成喷雾的粒度、平均和脉动速度,以及浓度进行了测量。研究了喷雾的结构,气流速度以及喷射方向对喷雾特性的影响,不同直径的粒子在横向的扩散。为两相流模型的研究以及数值计算结果的验证提供实验数据。      

基于Birge-Massart阈值降噪与EEMD及谱峭度的滚动轴承故障特征提取

针对传统共振解调方法易受噪声干扰导致故障特征提取效果不佳的问题,提出了一种基于Birge-Massart策略的阈值降噪与集成经验模态分解(EEMD)和快速谱峭度算法相结合的滚动轴承故障特征提取方法。对原始故障信号进行EEMD并采用峭度准则筛选出含有故障信息的本征模态函数(IMF)分量;采用Birge-Massart策略和快速谱峭度对故障信号进行滤波降噪;对滤波后信号进行Hilbert包络解调,提取轴承故障特征。采用该方法分别对仿真信号和实验信号进行特征提取,结果表明该方法可以有效提高故障信号信噪比,清晰准确地获取轴承内、外圈故障的频率特征。利用峭度因子准则筛选IMF分量能有效保留原始故障信号中的冲击特征,去除无关IMF分量的影响。      

Upstream Ion Cyclotron Waves at Venus and Mars

The occurrence of waves generated by pick-up of planetary neutrals by the solar wind around unmagnetized planets is an important indicator for the composition and evolution of planetary atmospheres. For Venus and Mars, long-term observations of the upstream magnetic field are now available and proton cyclotron waves have been reported by several spacecraft. Observations of these left-hand polarized waves at the local proton cyclotron frequency in the spacecraft frame are reviewed for their specific properties, generation mechanisms and consequences for the planetary exosphere. Comparison of the reported observations leads to a similar general wave occurrence at both planets, at comparable locations with respect to the planet. However, the waves at Mars are observed more frequently and for long durations of several hours; the cyclotron wave properties are more pronounced, with larger amplitudes, stronger left-hand polarization and higher coherence than at Venus. The geometrical configuration of the interplanetary magnetic field with respect to the solar wind velocity and the relative density of upstream pick-up protons to the background plasma are important parameters for wave generation. At Venus, where the relative exospheric pick-up ion density is low, wave generation was found to mainly take place under stable and quasi-parallel conditions of the magnetic field and the solar wind velocity. This is in agreement with theory, which predicts fast wave growth from the ion/ion beam instability under quasi-parallel conditions already for low relative pick-up ion density. At Mars, where the relative exospheric pick-up ion density is higher, upstream wave generation may also take place under stable conditions when the solar wind velocity and magnetic field are quasi-perpendicular. At both planets, the altitudes where upstream proton cyclotron waves were observed (8 Venus and 11 Mars radii) are comparable in terms of the bow shock nose distance of the planet, i.e. in terms of the size of the solar wind-planetary atmosphere interaction region. In summary, the upstream proton cyclotron wave observations demonstrate the strong similarity in the interaction of the outer exosphere of these unmagnetized planets with the solar wind upstream of the planetary bow shock.     

The Analyzer of Space Plasmas and Energetic Atoms (ASPERA-3) for the Mars Express Mission

The general scientific objective of the ASPERA-3 experiment is to study the solar wind – atmosphere interaction and to characterize the plasma and neutral gas environment with within the space near Mars through the use of energetic neutral atom (ENA) imaging and measuring local ion and electron plasma. The ASPERA-3 instrument comprises four sensors: two ENA sensors, one electron spectrometer, and one ion spectrometer. The Neutral Particle Imager (NPI) provides measurements of the integral ENA flux (0.1–60 keV) with no mass and energy resolution, but high angular resolution. The measurement principle is based on registering products (secondary ions, sputtered neutrals, reflected neutrals) of the ENA interaction with a graphite-coated surface. The Neutral Particle Detector (NPD) provides measurements of the ENA flux, resolving velocity (the hydrogen energy range is 0.1–10 keV) and mass (H and O) with a coarse angular resolution. The measurement principle is based on the surface reflection technique. The Electron Spectrometer (ELS) is a standard top-hat electrostatic analyzer in a very compact design which covers the energy range 0.01–20 keV. These three sensors are located on a scanning platform which provides scanning through 180^∘ of rotation. The instrument also contains an ion mass analyzer (IMA). Mechanically IMA is a separate unit connected by a cable to the ASPERA-3 main unit. IMA provides ion measurements in the energy range 0.01–36 keV/charge for the main ion components H⁺, He⁺⁺, He⁺, O⁺, and the group of molecular ions 20–80 amu/q. ASPERA-3 also includes its own DC/DC converters and digital processing unit (DPU).     

Target detection with synthetic aperture radar

Target detection with synthetic aperture radar (SAR) is considered. We derive generalized likelihood ratio (GLR) detection algorithms that may be used with SAR images that are obtained with coherent subtraction or have Gaussian distributions. We analytically compare the performance of (1) a single pixel detector, (2) a detector using complete knowledge of the target signature information and known orientation information, (3) a detector using incomplete knowledge of the target signature information and known orientation information (4) a detector using unknown target signature information and known orientation information, and (5) a detector using unknown target signature information and unknown orientation information     

In-flight Performance and Initial Results of Plasma Energy Angle and Composition Experiment (PACE) on SELENE (Kaguya)

MAP-PACE (MAgnetic field and Plasma experiment—Plasma energy Angle and Composition Experiment) on SELENE (Kaguya) has completed its ～1.5-year observation of low-energy charged particles around the Moon. MAP-PACE consists of 4 sensors: ESA (Electron Spectrum Analyzer)-S1, ESA-S2, IMA (Ion Mass Analyzer), and IEA (Ion Energy Analyzer). ESA-S1 and S2 measured the distribution function of low-energy electrons in the energy range 6 eV–9 keV and 9 eV–16 keV, respectively. IMA and IEA measured the distribution function of low-energy ions in the energy ranges 7 eV/q–28 keV/q and 7 eV/q–29 keV/q. All the sensors performed quite well as expected from the laboratory experiment carried out before launch. Since each sensor has a hemispherical field of view, two electron sensors and two ion sensors installed on the spacecraft panels opposite each other could cover the full 3-dimensional phase space of low-energy electrons and ions. One of the ion sensors IMA is an energy mass spectrometer. IMA measured mass-specific ion energy spectra that have never before been obtained at a 100 km altitude polar orbit around the Moon. The newly observed data show characteristic ion populations around the Moon. Besides the solar wind, MAP-PACE-IMA found four clearly distinguishable ion populations on the dayside of the Moon: (1) Solar wind protons backscattered at the lunar surface, (2) Solar wind protons reflected by magnetic anomalies on the lunar surface, (3) Reflected/backscattered protons picked-up by the solar wind, and (4) Ions originating from the lunar surface/lunar exosphere.     

The Earth's ring current: Causes,generation, and decay

The development of currents due to arbitrary distributions of trapped particles in the geomagnetic field is described. These currents form the Earth's ring current and are responsible for world wide decreases of the surface magnetic field observed during magnetic storms. It is shown that we do not yet know the relative abundances of the ions forming the ring current. Because of this we do not understand how various sources mix to produce the ring current. Several possible generation mechanisms are discussed. Finally, the decay of the ring current is discussed and is shown to be due primarily to charge exchange with important secondary effects attributable to wave-particle interactions.     

SACMA和QMW试验方法对复合材料层合板低速冲击后压缩行为的影响

采用了 SACMA标准和一种小试样试验方法对复合材料层合板低速冲击后的压缩 (CAI)行为进行试验研究 ,从层合板的冲击损伤分布、冲击后压缩破坏过程 ,以及层合板的准静态横向压缩、开孔后压缩等多方面进行对比 ,结果表明 ,这两种试验方法存在很大差别 ,试验方法不同 ,层合板低速冲击后的压缩行为也不同 ;采用 SACMA标准所测得的低速冲击后压缩强度更能全面反映基体韧性的优劣。作为 CAI试验标准 ,小试样试验方法还有待改进     

Three-dimensional plasma measurements within the earth's magnetosphere

First magnetospheric measurements of the three-dimensional velocity distributions for positive ions and electrons within the energy range 1 eV E/Q 45keV are reported. These velocity distributions are gained with quadrispherical Lepedeas on board the spacecraft ISEE-1 and -2. Three-dimensional bulk flows of protons in the vicinity of the magnetopause and within the dayside magnetosphere and dawn sector of the magnetotail are presented. Proton drift velocities within the magnetosphere and magnetotail can be directly determined and employed to calculate the corresponding quasi-static perpendicular electric fields and to provide quantitative analyses of kinematical models for plasma motions. Nonmonotonic features in the electron velocity distributions are found simultaneously with the presence of electron cyclotron harmonic electrostatic waves in the dayside magnetosphere. The relationship of the observed electron velocity distributions to expectations for resonant pitch-angle and energy diffusion is discussed, as well as the possibility of the existence of proton cyclotron harmonic instabilities. Examples of the signature of field-aligned acceleration of protons into the magnetosphere and the presence of low-energy ionospheric ions in the near-earth magnetotail are also presented. Perpendicular electrostatic fields can be calculated from the observed three-dimensional velocity distributions and are found to have typical magnitudes of 1 mV m^-1.     

The local interstellar medium viewed through pickup ions, recent results and future perspectives

Over the last 10 years the experimental basis for the study of the very local interstellar medium (VLISM) has been substantially broadened by the direct detection of pickup ions and of neutral helium. The strength of these methods lies in the local measurement of the particles. By scanning the gravitational focusing cone of the interstellar wind, a consistent set of interstellar helium parameters, neutral density, temperature and relative velocity, has been derived. However, the accuracy of these parameters is still hampered by uncertainties in some of the crucial ionization rates and in the pickup ion transport. Recent observations have shown that the scattering mean free path of pickup ions is comparable with the large scale variation of the interplanetary magnetic field (IMF) in the inner heliosphere. This requires a substantial modification in the modeling of the ion distribution and more detailed measurements, tasks that can be addressed in the near future.     

Influence of the Interplanetary Magnetic Field on the Solar Wind Flow about Planetary Obstacles

The main effects caused by the interplanetary magnetic field (IMF) are analyzed in cases of supersonic solar wind flow around magnetized planets (like Earth) and nonmagnetized (like Venus) planets. The IMF has a relatively weak strength in the solar wind but it is enhanced considerably in the so-called plasma depletion layer or magnetic barrier in the vicinity of the streamlined obstacle (magnetopause of a magnetized planet, or ionopause of a nonmagnetized planet). For magnetized planets, the magnetic barrier is a source of free magnetic energy for magnetic reconnection in cases of large magnetic shear at the magnetopause. For nonmagnetized planets, mass loading of the ionospheric particles is very important. The new created ions are accelerated by the electric field related to the IMF, and thus they gain energy from the solar wind plasma. These ions form the boundary layer within the magnetic barrier. This mass loading process affects considerably the profiles of the magnetic field and plasma parameters in the flow region.     

燃气源开槽导管三维流场的数值模拟

为了解某火箭弹控制系统燃气源开槽导管内的气流流动特性,通过ＳＩＭＰＬＥ方法对其复杂流场进行了数值模拟。采用隐式时间分裂格式、幂函数方案及交错网格修正压力等方法,获得了燃烧室后部和导管内气流的速度、压力、密度和温度的三维分布,计算结果与实验现象的规律一致     

民用飞机综合模块化航电系统分区和资源分配的研究

对比航电传统系统架构,分析了综合模块化航电系统(Integrated Modular Avionics,简称IMA)架构的优点;针对IMA系统功能的高集成度带来的资源分配难度和安全性要求,提出了IMA系统分区和资源分配策略,并给出了具体方法,对民用飞机IMA系统设计具有一定的指导意义和实用价值。     

民用飞机综合模块化航电系统资源状态监控技术研究

随着处理器和机载嵌入式实时分区操作系统等相关技术的不断升级换代,IMA系统功能的集成度也越来越高,高集成度增加了系统资源分配的难度,需要通过对系统资源状态进行实时监控和分析进而不断优化系统配置。首先对IMA系统的分区特性进行了深入研究,基于探针插桩监控数据采集技术,提出了一种系统行为和时间资源状态监控的策略。研究了数据监控采集系统的软件架构,在此基础上设计和实现了系统行为监视器和时间资源监视器,并在某民机重点预研课题中进行了应用验证。结果表明,能够有效帮助应用开发者和系统综合者直观分析系统时间性能瓶颈,优化资源配置方案,实现计算资源的负载均衡。对IMA系统资源状态监控及资源配置优化具有一定的指导意义和实用价值。