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．     

远程教学网站的建设与管理

远程教学是当前地方党校系统普遍采用的一种新型教育教学方式,包括中央党校远程教学和农村党员远程教育.对中央党校远程教学网站的利用,可以采用"点课"、"辅导"、"大报告"等模式;对农村党员远程教育网站的利用,应重点考虑该站视频节目的应用.     

基于着色Petri网的航空发动机总装作业调度研究

针对航空发动机作业并行交叉的特点,提出一种“自底向上”的柔性建模方法,着重描述异类对象作业工序对资源的占用与冲突。引入基于资源库所的共享合成运算,解决了Petri网结构重用性差而无法动态建模的问题,合成模型具有守衡、有界和无死锁的结构性质。模型的状态方程在极大-加法代数意义下具有线性的形式,结合遗传算法实现基于周期的静态调度优化。     

陶瓷纤维梯度增强活塞的梯度方程研究

 功能梯度材料零件具有单质材料零件无法比拟的理化性能优势,然而由于材料分布复杂以及对功能梯度材料本身性能研究不充分,使性能分析存在很多困难。论文应用复合材料热性能理论,采用有限元分析软件ADINA,分析陶瓷纤维梯度增强活塞（材料梯度方程的参数不同）的温度分布和应力分布,结果表明陶瓷纤维梯度层可以明显改变活塞温度分布,缓和由于热膨胀系数不匹配,在陶瓷纤维增强层与活塞本体交界处产生的应力。根据计算结果拟合出温度峰值、整体应力峰值和层间应力峰值与方程系数之间的曲线,并加以验证。     

燃料组分差异对贫油熄火边界的影响

为了推进替代燃料的多元化,扩大航空燃料的组分分布。以标准航空煤油为基准,研究了柴油和高沸点费托油对燃烧室贫油熄火边界的影响。实验采用单头部燃烧室,通过改变燃烧室进出口压力,研究其熄火边界的变化规律,并分析了其与理化性质和组成的关联关系。结果显示在220kPa的出口压力下,航空煤油的熄火性能略优于另外两种燃油,高沸点费托油相比航空煤油熄火边界窄5%,而在140kPa的低压条件下,高沸点费托油的熄火边界相比航空煤油拓宽了8%。分析得到整体上低沸点烷烃和直链烷烃的熄火性能较好。      

替代燃料贫油熄火边界影响因素

为了研究燃油以及入口空气压力对于贫油熄火(LBO)边界的影响大小及规律,采用航空煤油(RP-3)、高沸点费托油(FT)和柴油进行了三种不同燃烧室入口压力工况下的贫油熄火实验并进行规律分析。分析结果表明:入口压力对贫油熄火边界的影响(19.17%)要大于燃油性质造成的影响(6.26%)。导致熄火油气比变化的主要因素包括入口空气压力,火焰体积,燃烧室温度,燃油雾化直径以及燃油的热值和密度,其中火焰体积和燃油雾化直径主要受燃油性质影响,而燃烧室温度则与入口压力有很大关系。入口压力影响的贫油熄火油气比变化会受其影响的火焰体积和燃烧室温度变化而削弱。碳数高支链烷烃含量少的燃油可能会提高火焰体积对熄火油气比的影响,使其在低入口压力下有更好的贫油熄火边界。      

LD10网格加强肋结构壁板的化学铣切工艺研究

为了寻找到化铣槽液各组分的最佳含量范围,使零件达到稳定化铣侧切率,减少板材铣切厚度差,本研究通过测量对比试片在各组分含量的槽液中铣切壁板的侧切率和均匀度参数来实现.结果表明,当NaOH初始浓度为200 g/L、溶解Al3+为70～110 g/L、温度(90±5)℃的技术条件下能够得到肋条偏差Tw±0.75 mm、壁厚偏差Ts±0.15 mm的较理想的化铣产品.