What Determines the Composition of SEPs in Gradual Events?

Gradual solar energetic particle (SEP) events are evidently accelerated by coronal/interplanetary shocks driven by coronal mass ejections. This talk addresses the different factors which determine the composition of the accelerated ions. The first factor is the set of available seed populations including the solar wind core and suprathermal tail, remnant impulsive events from preceding solar flares, and remnant gradual events. The second factor is the fractionation of the seed ions by the injection process, that is, what fraction of the ions are extracted by the shock to participate in diffusive shock acceleration. Injection is a controversial topic since it depends on the detailed electromagnetic structure of the shock transition and the transport of ions in these structured fields, both of which are not well understood or determined theoretically. The third factor is fractionation during the acceleration process, due to the dependence of ion transport in the turbulent electromagnetic fields adjacent to the shock on the mass/charge ratio. Of crucial importance in the last two factors is the magnetic obliquity of the shock. The form of the proton-excited hydromagnetic wave spectrum is also important. Finally, more subtle effects on ion composition arise from the superposition of ion contributions over the time history of the shock along the observer’s magnetic flux tube, and the sequence of flux tubes sampled by the observer.     

低频声波对水雾消散作用的实验研究

作者考查了低频声波(<50Hz)对于水雾消散的作用。通过建立声波消雾实验装置,测定了在水雾消散过程中,雾室内的声场分布、温度、消雾时间、雾滴谱的变化过程。实验结果表明声波作用对于水雾的消散具有明显的作用。并且,消雾的效果随着作用声波的频率和声压级(SPL)呈规律性的变化趋势。较低频率和较高声强的声波作用更有利于水雾的消散,在消雾的过程中温度起伏不大。而声致凝聚是声波消雾的主要因素之一。     

基于因子模糊化BP神经网络的磨损颗粒识别

在引入了一套磨粒形态学描述子来提取磨损颗粒的显微形态特征的基础上 ,采用人工神经网络技术 ,编制了用于磨损颗粒自动识别的 BP网络计算机模拟程序。在网络训练的过程中应用了本文引入的因子模糊化训练方法 ,使训练速度大大加快 ,以异或问题为例 ,速度可提高 5～ 1 0倍。应用此网络对磨粒测试库进行识别实验 ,识别正确率在 90 %以上 ,并且识别速度很快 ,大大优于传统的磨粒识别方法。     

稀土对电沉积镍基复合镀层高温抗氧化性的影响

研究了稀土加入三种电沉积镍基复合镀层Ni—B_4C、Ni—TiC、Ni—ZrO_2前后,在850℃时的氧化行为。通过金相观察、ESCA(光电子能谱)分析及X射线衍射等方法研究表明:镀层中不同的复合颗粒和稀土两者对镀层的抗氧化能力均有影响。其小不同种类的颗粒对镀层抗氧化能力所产生影响的差别很明显;而稀土对镀层抗氧化能力影响的差别较小,且影响的程度比较接近。另外,两者影响的机理也不同。颗粒是通过分解、扩散等过程改变表面膜的组成来影响的,而稀土则是从提高膜的致密度和膜与基体的粘附性来影响的。作者认为,它们的影响既互相独立,而又互相补充。     

航天器总装多余物控制方法探讨

带有多余的航天产品存在重大的质量事故隐患。文章对航天器总装中的多余物进行了分类,从而分析多余物产生的机理有4大来源:总装工艺过程、零组件及人员带入、贮存过程、有害气体。介绍了多余物的危害,提出了系统控制多余物的思路和多余物常用检查及排除的方法。     

IMF connection for energetic protons observed at Ulysses via mid-latitude solar wind rarefaction regions

As Ulysses moved inward and southward from mid-1992 to early 1994 we noticed the occasional occurrence of inter-events, lasting about 10 days and falling between the recurrent events, observed at proton energies of 0.48–97 MeV, associated with Corotating Interaction Regions (CIR). These inter-events were present for several sequences of two or more solar rotations at intensity levels around 1% of those of the neighbouring main events. When we compared the Ulysses events with those measured on IMP-8 at 1 AU we saw that the inter-events appeared at Ulysses after the extended emission (>10 days) of large fluxes of solar protons of the same energy that lasted at least one solar rotation at 1 AU. The inter-events fell completely within the rarefaction regions (dv/dt<0) of the recurrent solar wind streams. The interplanetary magnetic field (IMF) lines in the rarefactions map back to the narrow range of longitudes at the Sun which mark the eastern edge of the source region of the high speed stream. Thus the inter-events are propagating at mid-latitudes to Ulysses along field lines free from stream-stream interactions. They are seen in the 0.39–1.28 MeV/nucleon He, which exhibit a faster decay, but almost never in the 38–53 keV electrons. We show that the inter-events are unlikely to be accelerated by reverse shocks associated with the CIRs and that they are more likely to be accelerated by sequences of solar events and transported along the IMF in the rarefactions of the solar wind streams.     

固体火箭喷管排气中的粒子分布

1.前言 现代的固体火箭发动机为提高推进剂的能量特性及抑制不稳定燃烧，常常在推进剂中添加金属粉末，最常见的是加金属铝粉。在发动机工作时，铝粉燃烧形成凝聚相的氧化铝粒子。这些粒子在喷管中的流动过程中，温度、速度等方面的变化滞后于燃·气本身的变     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.     

基于光滑粒子流体动力学方法的液滴蒸发问题数值模拟研究

基于光滑粒子流体动力学方法（Smoothed Particle Hydrodynamics，SPH），开展了SPH新算法在蒸发燃烧领域的研究。建立了适用于SPH方法的蒸发数值模型，推导了基于傅立叶热传导公式和菲克扩散定律的SPH离散方程；借鉴VOF方法（Volume of Fluid）的思想，提出了SPH粒子的液相质量分数的概念，以有效表征蒸发过程中的相变问题。采用SPH方法对高温环境中单个液滴的蒸发过程进行数值模拟，结果符合D2定律，与理论模型相一致；在强迫对流环境中，液滴的蒸发过程受到对流作用及表面张力的影响，蒸发速率加快；进一步对双液滴在静止、对流环境中的蒸发过程进行数值模拟研究。结果表明，液滴的间距、滴径对多个液滴的蒸发过程影响至关重要，液滴间距至少在两倍的液滴直径以上，相互之间的影响才可以近似忽略。通过本文研究，拓宽了SPH方法在蒸发相变领域的应用范围，研究结果也能够为进一步的燃烧问题研究奠定基础。     

流变铸造法制备Al_2O_（3P）／ZA4－3复合材料的研究

为提高模用锌合金ＺＡ４－３的性能，扩大其应用范围，本项工作采用流变铸造法成功地制备了性能稳定的Ａｌ２Ｏ３Ｐ／ＺＡ４－３复合材料。对该材料进行了弯曲强度、冲击韧性、压缩强度、硬度及耐磨性等性能试验，结果表明：Ａｌ２Ｏ３ｐ的加入，使锌合金的压缩强度、室温和高温硬度以及耐磨性明显提高，其弯曲强度略有降低，而其冲击韧性下降了　。最后还讨论了成形工艺参数、颗粒含量和颗粒直径对该复合材料性能的影响。