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.     

混粉电火花加工表面的研究

分析了混粉电火花加工工件表面的组成成分,探讨了混粉电火花加工获得低的表面粗糙度的机理。     

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.     

模拟月壤研制的初步设想

模拟月壤是月球样品的地球化学复制品，作者总结世界上已有的5种模拟月壤JSC-1，MLS．1，MLS-2，MKS-1和FJS-1的研制过程、方法与基本理化性质，认为系列化模拟月壤研制对中国首次月球探测有重要意义，在此基础上，作者提出系列化模拟月壤研制的基本思路．     

Si和Ti对Nb-6Hf-4Zr-2B合金组织和室温力学性能的影响

 为了寻求Nb合金的强度和塑性的平衡,设计了以Nb基固溶体Nbss为主导相的Nb-xSi-6Hf-4Zr-2B-yTi(x=4,8;y=10,30;原子分数)合金,研究了Si和Ti对合金组织和室温力学性能的影响。结果表明,合金由Nbss、Nb3Si和Nb5Si3等3相组成。4Si-(10,30)Ti合金铸态组织是Nb枝晶和分布在枝晶间的硅化物(Nb3Si和Nb5Si3),8Si-(10,30)Ti合金Nb枝晶间分布的是Nb/硅化物(Nb5Si3)的共晶和Nb3Si,随着Si和Ti含量的增加,硅化物体积分数增加。1 600 ℃退火50 h可使部分Nb3Si共析分解,改变合金的组织形貌和各相的体积分数。随着Si和Ti含量的增加,合金的硬度和强度增加,但塑性和韧性降低。Nb枝晶的失效方式为解理断裂,而硅化物为脆性断裂。     

电子束物理气相沉积YSZ热障涂层热循环性能

考察了YSZ热障涂层的抗热循环性能;分别利用SEM、XRD分析了热循环前后涂层的显微结构和相组成。经分析可知,YSZ热障涂层具有典型的柱状晶结构,沉积态时YSZ涂层为t/t′相,经过600次热循环后,YSZ涂层未发现脱落。     

TC11钛合金钨极氩弧焊工艺试验研究

针对TC11钛合金材料进行了自动钨极氩孤焊接工艺试验,获得了成形良好的焊缝,焊接质量符合航空Ⅰ级焊缝标准.采用金相试验方法和力学性能试验对不同焊接填充材料下的显微组织和性能进行对比.结果表明,采用TC11同质焊丝可获得与母材抗拉强度相当的焊接接头,略高于采用TA2纯钛焊丝的接头,但采用TA2焊丝时的集中塑性接近母材.     

镍基单晶高温合金的发展

概述了镍基单晶高温合金的发展历程,分析了其成分、相组成、热处理的特征和持久变形及强化机制,给出了其持久性能数据,并指出了发展趋势。     

燃烧室进油管焊缝裂纹失效分析

燃烧室进油管沿周圈出现开裂现象,对它进行外观检查、断口分析、冶金分析及综合分析,结果表明燃烧室进油管在氩弧焊焊接过程中由于焊接不当,导致在焊缝收弧处产生焊接缺陷——咬边及焊瘤,且焊缝处于尺寸变化较大的部位,容易产生应力集中,在工作过程中萌生裂纹并疲劳扩展。     

面向对地成像观测任务的高空飞艇应急调度

针对应急条件下高空飞艇(HAA)对地成像观测任务调度问题进行研究,分析了问题中的主要约束条件,建立了以任务收益(TB)和巡航距离为优化目标的约束满足问题(CSP)模型。考虑飞艇侦察载荷具有侧摆观测能力,在构建视场范围约束模型和分辨率约束模型的基础上,对成像观测任务进行合成。提出了元任务与合成任务的概念,给出了任务合成的步骤与方法。将HAA应急调度问题转换为车辆路径问题(VRP),并进一步分解为任务排序主问题和路径选择子问题,分别应用改进粒子群(IPSO)算法和关键节点搜索(KNS)算法求解。详细介绍了算法中的编码、解码和移动等操作,以及采用的混沌初始化和禁忌搜索(TS)策略。通过仿真实验,对文中所提方法的有效性进行了验证。