羽流场与月壤颗粒相互作用的一种新计算方法

针对登月着陆器发动机下降过程中羽流场与月壤颗粒相互作用问题提出了一种新的计算方法。通过Morh\|Coulomb破坏准则确定月壤颗粒可以被羽流扬起的临界剪应力,采用动量原理计算被扬起的月壤颗粒的质量大小及形成的月坑深度;基于牛顿第二定律,采用羽流场与月壤颗粒的流固耦合相互迭代的计算方法,获得被扬起月壤颗粒随时间的质量分布等。本文通过美国Apollo 11登月过程实测数据对该新方法进行了验证,为人类探月工程提供一定数据参考。     

过载下燃烧室粒子特性与绝热层烧蚀研究进展

总结和分析了国、内外对飞行过载下固体火箭发动机中出现的绝热层烧蚀问题的研究方法。详细阐述了燃烧室粒子粒度参数确定方法、过载流场数值模拟方法及地面模拟过载试验方法等方面研究进展。首次提出了获取过载下粒子分布参数的两种新途径,即基于飞行发动机的粒子收集分析法与故障位置反算分析法,给出了两种方法下的粒度分布参数;并提出了用火箭橇模拟过载下绝热层烧蚀的方法。结合某战术发动机,基于过载流场计算结果,讨论了短时间大过载与长时间中、小过载等两种典型工况对绝热层的烧蚀影响,并给出了热防护设计时应注意的问题。     

直升机粒子分离器三维两相流场的数值模拟

本文以某型直升机粒子分离器为研究对象, 在三维非正交曲线坐标系下计算湍流分叉流动和砂粒运动, 结合边界条件特殊处理, 采用分块计算来考虑叶片对流场的影响, 首次对有叶片粒子分离器三维两相流动进行了数值模拟。      

GH4169G合金零件异常腐蚀区缺陷分析

针对生产中GH4169G合金零件低倍全面腐蚀时出现的异常腐蚀区,采用光学显微镜、扫描电子显微镜及能量散射谱,对正常区域和异常腐蚀区的宏观、微观组织形貌及化学成分进行了对比分析。结果表明,异常腐蚀区为白斑缺陷;虽然该异常腐蚀区离散分布着富Ca和富Mg的氧化物颗粒,但氧化物颗粒未见聚集,由此判断该缺陷为"干净"白斑。强度类比评估表明,带白斑缺陷零件可满足阶段性试验要求,且试验后分解检查未发现零件异常。     

基于产物分析的铁粉燃烧器燃烧特性实验研究

铁粉是一种潜在的绿色可再生金属燃料。为了探索铁粉燃料使用的可行性,改进铁粉燃烧器的设计方法,研究铁粉的燃烧特性,进而实现铁粉燃烧后能量的有效利用,文中采用自主设计的金属铁粉燃烧器,实现了铁粉与空气在常压下的自持燃烧,进一步研究了铁颗粒燃烧后产物的变化规律。在点火燃烧实验中发现,铁粉的最佳点火浓度条件在0.95～1.28kg/m³。利用扫描电子显微镜（SEM）、激光粒度分析仪（LPSA）、聚焦离子束（FIB）和X射线衍射（XRD）等诊断手段对燃烧产物进行了分析。结果表明,铁颗粒燃烧后颗粒形貌由不规则形最终变成球形,在燃烧过程中生成的产物会直接包裹在金属液滴的表面导致产物的粒度增大,在空燃比为0.55时,粒度的增大率为1.2,富燃条件下,随着空燃比的提高,产物的增大率变大。使用相图预测了铁颗粒在燃烧过程中出现的多层结构,利用FIB方法进一步分析了铁颗粒在燃烧反应中间阶段的层结构由外向内分别为Fe₂O₃,Fe₃O₄,FeO和Fe。     

Energetic particle signatures of geoeffective coronal mass ejections

We have studied statistically associations of moderate and intense geomagnetic storms with coronal mass ejections (CMEs) and energetic particle events. The goal was to identify specific energetic particle signatures, which could be used to improve the predictions of the geoeffectiveness of full and partial halo CMEs. Protons in the range 1–110 MeV from the ERNE experiment onboard SOHO are used in the analysis. The study covers the time period from August 1996 to July 2000. We demonstrate the feasibility of energetic particle observations as an additional source of information in evaluating the geoeffectiveness of full and partial halo CMEs. Based on the observed onset times of solar energetic particle (SEP) events and energetic storm particle (ESP) events, we derive a proxy for the transit times of shocks driven by the interplanetary counterparts of coronal mass ejections from the Sun to the Earth. For a limited number of geomagnetic storms which can be associated to both SEP and ESP signatures, we found that this transit time correlates with the strength of geomagnetic storms.     

Solar proton enhancements in different energy channels and coronal mass ejections during the last solar cycle

The main properties of 11622 coronal mass ejections (CMEs) observed by the Solar and Heliospheric Observatory (SOHO) mission’s Large Angle and Spectrometric Coronagraph (LASCO-C2) from January 1996 through December 2006 are considered. Moreover, the extended database of solar proton enhancements (SPEs) with proton flux >0.1 pfu at energy >10 MeV measured at the Earth’s orbit is also studied. A comparison of these databases gives new results concerning the sources and acceleration mechanisms of solar energetic particles. Specifically, coronal mass ejections with width >180° (wide) and linear speed >800 km/s (fast) seem they have the best correlation with solar proton enhancements. The study of some specific solar parameters, such as soft X-ray flares, sunspot numbers, solar flare index etc. has showed that the soft X-ray flares with importance >M5 may provide a reasonable proxy index for the SPE production rate. From this work, it is outlined that the good relation of the fast and wide coronal mass ejections to proton enhancements seems to lead to a similar conclusion. In spite of the fact that in the case of CMEs the statistics cover only the last solar cycle, while the measurements of SXR flares are extended over three solar cycles, it is obvious for the studied period that the coronal mass ejections can also provide a good index for the solar proton production.     

PDPA与HW测量技术的对比试验研究

利用自由剪切湍流中的圆管射流所具有的流动特性,采用相位多普勒粒子分析仪（ＰｈａｓｅＤｏｐｐｌｅｒＰａｒｔｉｃｌｅＡｎａｌｙｚｅｒ）对射流随轴向发展的最大速度进行了７次重复性测量试验,给出非侵入测量射流的势流区和湍流自模拟区的测量精度。文中还进行了热线与ＰＤＰＡ对射流最大速度随轴向衰减变化的测量试验,给出了ＰＤＰＡ与ＨＷ测量结果之间的关系曲线和公式。同时给出了侵入测量中探头对流场中当地速度的干扰影响量。     

掺杂物形状对混合粒子等效光学常数的影响

基于电磁场平均的概念,利用Maxwell-Garnett有效介质理论对含有椭球形掺杂物的混合粒子等效光学常数进行研究,分析了掺杂物形状比例参数和体积分数对混合粒子等效光学常数的影响.结果表明:掺杂物形状比例参数存在一个临界值,当形状比例参数小于临界值时,随着形状比例参数增加,含椭球形掺杂物的混合粒子等效光学常数与含球形掺杂物的混合粒子等效光学常数的差别增大;反之,形状比例参数对混合粒子等效光学常数的影响非常小.混合粒子的等效光学常数介于基体和掺杂物的光学常数之间,当掺杂物的体积分数增大时,混合粒子的等效光学常数趋向于掺杂物的光学常数.      

Radiation from relativistic shocks in turbulent magnetic fields

Using our new 3-D relativistic particle-in-cell (PIC) code parallelized with MPI, we investigated long-term particle acceleration associated with a relativistic electron–positron jet propagating in an unmagnetized ambient electron–positron plasma. The simulations were performed using a much longer simulation system than our previous simulations in order to investigate the full nonlinear stage of the Weibel instability and its particle acceleration mechanism. Cold jet electrons are thermalized and ambient electrons are accelerated in the resulting shocks. Acceleration of ambient electrons leads to a maximum ambient electron density three times larger than the original value as predicted by hydrodynamic shock compression. In the jet (reverse) shock behind the bow (forward) shock the strongest electromagnetic fields are generated. These fields may lead to time dependent afterglow emission. In order to calculate radiation from first principles that goes beyond the standard synchrotron model used in astrophysical objects we have used PIC simulations. Initially we calculated radiation from electrons propagating in a uniform parallel magnetic field to verify the technique. We then used the technique to calculate emission from electrons in a small simulation system. From these simulations we obtained spectra which are consistent with those generated from electrons propagating in turbulent magnetic fields with red noise. This turbulent magnetic field is similar to the magnetic field generated at an early nonlinear stage of the Weibel instability. A fully developed shock within a larger simulation system may generate a jitter/synchrotron spectrum.