分级/预混合预蒸发贫油燃烧低污染方案NOX排放初步研究

对分级/贫油预混合预蒸发低污染燃烧方案的氮氧化物排放进行了初步试验研究,主要目的是考察贫油预混合预蒸发级降低污染排放的能力。预燃级是常规双涡流器空气雾化喷嘴,主燃级是空气雾化喷嘴雾化燃油,配装蒸发管,头部涡流器组织燃烧。燃油为RP-3航空煤油。采用单头部燃烧室,工况模拟了燃烧室进口温度(800K)、进口速度和总油气比,压力为常压。研究结果表明,旋流式贫油预混合预蒸发燃烧的主燃级有降低氮氧化物的潜力,相对于常规燃烧组织方式,能够降低NO_X排放量为60%,同时发现,燃油分级比例对NO_X降低也有很大影响。      

灰色理论在垃圾气化过程中NOx排放定量预测的应用

本文把灰色理论及方法应用于对垃圾气化处理的NOx排放的定量预测中。建立了一定工况条件下的垃圾气化处理中的NOx排放的灰色预测模型。所建模型的预测结果与实际值的误差只有1％左右。通过本文的实例表明，该方法具有预测精度高、简便易行的优点。对固体废物的气化处理过程中的污染物排放控制具有指导意义。     

汽车发动机燃烧代用燃料的主要问题

本文较全面地概述了主要代用燃料的物化特性、燃用经济性、排放试验对比结果和有关技术问题,简述了国内外燃用代用燃料的发展状况。文中指出燃用代用燃料对节能、环保、开发新能源的重要意义,以及燃用代用燃料时发动机结构的改变。     

确定飞机日历寿命用的当量环境谱研究

提出了飞机使用环境由机场湿热大气环境、水介质浸泡环境和热空气老化环境三部分所组成;根据损伤等效原则,由法拉第定律和阿伦尼斯方程,分别推导出一套不同环境之间的当量化关系式;在环境实测和试验的基础上,建立了一种适用于飞机关键部位的加速腐蚀试验环境谱,并成功地确定了某机场的当量环境谱。     

Relative ionizations in the nearest interstellar gas

We compare CLOUDY predictions for the equilibrium ionization in the interstellar cloud surrounding the solar system with pick-up ion data. The incident radiation field includes contributions from hot stars, the emission from the conductive cloud boundary and the diffuse FUV back-ground. To within the observational uncertainties, CLOUDY predictions for the ratios n(He)/n(O), n(N)/n(O), n(Ne)/n(O), and n(He)/n(Ne) are consistent with pick-up ion data, provided that O and N are filtered by 50% in the heliopause region and the outer heliosphere as predicted by others. Thus, the steady-state ionization model and assumed radiation field appear approximately valid. However, the youth and low intervening column density towards the Vela pulsar leave open the possibility that the parent supernova explosion 10,500 years ago, and 200 pc distant, may also have affected LISM ionization, although the mechanism is uncertain. Support for this last possibility is provided by the apparent signature of the Vela explosion in the terrestrial geological record.Abbreviations ISM Interstellar Medium - FUV Far Ultraviolet - EUV Extreme Ultraviolet - SNR SN remnant - SXRB SXR Background - LISM Local Interstellar Matter     

弯掠动叶旋转失速工况下气动声学的实验分析与计算

测量了轴流式弯掠动叶和径向动叶在旋转失速工况下的气动噪声和噪声频谱，实验结果表明：弯掠动叶能够降低气动噪声。讨论了弯掠动叶对宽频噪声和离散噪声的影响，并且得到了适于计算弯掠动叶旋转失速工况的气动噪声计算方法。     

Manifestation of magnetic reconnection in coronal streamer current sheets

We investigate the possibility of observing the effects of magnetic reconnection inside a current sheet forming in a coronal streamer in the extended corona. In particular we study the possibility to observe with the UVCS of SOHO the excitation of the tearing instability in the current sheet.     

飞机结构设计阶段估算谱载下裂纹扩展模型参数的优化方法

提出在短周期谱载荷下,飞机结构设计阶段,裂纹扩展模型ｄａ／ｄｔ＝Ｑａｂ参数的估算法,此法可以依据材料参数、载荷谱和结构的几何特征使用优化设计方法计算。     

飞机空中使用环境谱的编制

 空中环境谱是飞机使用环境谱的重要组成部分。首先对影响飞机结构完整性的污染物元素浓度进行了空测,其次应用模糊聚类理论确定了空中环境谱的水平区域尺度大约为200 km,高度区域尺度大约为2 km,最后应用SPSS统计软件研究了污染物元素浓度随高度的分布规律,得到了统计意义上的预测模型,预测结果与实测结果有“较好”的一致性。     

An Update on Ultra-Heavy Elements in Solar Energetic Particles above 10 MeV/Nucleon

Measurements below several MeV/nucleon from Wind/LEMT and ACE/ULEIS show that elements heavier than Zn (Z=30) can be enhanced by factors of ∼100 to 1000, depending on species, in ³He-rich solar energetic particle (SEP) events. Using the Solar Isotope Spectrometer (SIS) on ACE we find that even large SEP (LSEP) shock-accelerated events at energies from ∼10 to >100 MeV/nucleon are often very iron rich and might contain admixtures of flare seed material. Studies of ultra-heavy (UH) SEPs (with Z>30) above 10 MeV/nucleon can be used to test models of acceleration and abundance enhancements in both LSEP and ³He-rich events. We find that the long-term average composition for elements from Z=30 to 40 is similar to standard solar system values, but there is considerable event-to-event variability. Although most of the UH fluence arrives during LSEP events, UH abundances are relatively more enhanced in ³He-rich events, with the (34<Z<40)/O ratio on average more than 50 times higher in ³He-rich events than in LSEP events. At energies >10 MeV/nucleon, the most extreme event in terms of UH composition detected so far took place on 23 July 2004 and had a (34<Z<40)/O enhancement of ∼250–300 times the standard solar value.