浮动壁火焰筒壁温试验和计算分析

对某浮动壁火焰筒的壁温进行了试验和计算分析。该火焰筒应用了新型的浮动壁结构和高效的冲击/发散复合冷却技术。壁温分布试验在全环形燃烧室试验台上进行,采用热电偶和示温漆测量。计算采用了稳态导热问题的有限元求解方法。研究分析表明,火焰筒壁温在材料的长期许用温度范围内,壁温计算反映了火焰筒壁温的分布规律和趋势。冲击/发散复合冷却方式的轴向壁温梯度小于缝槽气膜冷却方式,对降低热应力水平,延长火焰筒使用寿命有利。     

N2O-C2H2火焰原子吸收光谱法测定纯镍中硅含量

为简化纯镍中硅含量的测定过程,提高测量精度,研究了一种N2O-C2H2火焰原子吸收光谱法用于检测。介绍了方法的原理、工作参数和测定条件,并确定最佳工作条件,讨论了燃烧温度、共存离子等干扰因素的影响。实验结果表明,该法的灵敏度高、干扰小、选择性和重现性好,操作简单,分析周期短。其测定结果的相对标准偏差均小于1.0%,标准加入回收率大于97.0%(样本数n=6),可满足实验室仪器分析质量与控制的要求。     

谐振腔光纤陀螺频率调制原理及仿真

简述对谐振腔光纤陀螺入射光进行频率调制的基本方法，采用洛仑兹公式来描述光纤陀螺的传递函数，结合输入信号特征，建立其频域的数学模型，最后给出结果和相关仿真图形，以及关键参数的优化值和优化方向，再对全光路的结构提出具体的配置建议，仿真结果表明，谐振腔光纤陀螺具有良好的线性工作区间，精度也能够得到进一步的提高。     

环形火焰引发爆震的数值研究

采用改进的适于多组分反应流的波传播算法,对直管道中甲烷．空气预混气的爆震引发过程进行数值研究,考虑了两种不同构型的初始环形火焰对引发爆震的影响。对这两种构型下爆震引发过程中的压力场、温度场、反应放热率以及组分浓度进行了计算,由此探讨了“热点”形成机制及其对爆震引发的作用。结果表明,火焰发展产生的燃烧压缩波在管壁或管轴心发生汇聚、碰撞所形成的复杂波系与火焰相互作用,导致火焰前锋与压缩波之间的局部区域反应剧烈,反应放热率明显增加,从而促使热点形成。形成的热点迅速放大成为过驱爆震波,并逐渐衰减为稳定爆震波。稳定爆震波阵面参数与CJ理论结果进行了对比,两者符合得较好。     

非像面散斑法层析火焰折射率场分布

本文通过理论分析给出了激光束通过火焰后的偏转角与折射率的关系，并给出了透镜后非像面散斑与火焰周围介质折射率场的关系表达式。用双曝光散斑法层析了火焰上不同截面的折射率分布。给出实验结果，并予以讨论。     

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.     

新型内突扩加力燃烧室方案可行性分析

介绍了一种新型内突扩加力燃烧室方案,具有质量轻、尺寸小、红外隐身功能突出等优点;在分析当前高推重比发动机需求的基础上,结合目前国内外加力燃烧室的技术水平,根据新一代军用发动机的加力燃烧室进气参数,论证了该方案所具有的现实可行性。     

高温升火焰筒壁面及头部复合冷却设计分析

某燃烧室火焰筒壁面采用冲击＋逆向对流＋气膜冷却技术，火焰筒头部采用冲击＋对流冷却技术。本文通过计算并与试验结果对比分析表明：该火焰筒的冷却设计基本合理、可行，经进一步的改进和完善后。可作为高温升燃烧室火焰筒的优选设计方案之一。     

煤油超燃冲压发动机两相流场数值研究 (Ⅲ)煤油在超燃流场中的多步化学反应特征

深入分析了煤油代用燃料C12H23的17组分30步反应模型在超燃冲压发动机流场内的细观化学反应动力学特征,结果表明：(1)该化学反应模型比较合理地描述了煤油在超燃流场内的裂解、点火、裂解产物的燃烧以及和NOx的生成等基本规律和特征,其中对于OH分布特征的预示和文献的利用PLIF的物理观测结果一致。不过,其单步裂解机制对温度场的预估偏高。(2)对导流型凹槽内的化学动力学特征分析表明,导流槽由于加强了凹槽外氧气向凹槽内的输运,使得凹槽内的燃烧得以强化,生成的CO2偏多。(3)煤油的化学反应动力学过程对于准确预示和评价煤油在超燃发动机内的燃烧状况及发动机整体性能有重要影响。     

高温富油燃气作引导火焰的煤油超燃研究

对采用高温富油燃气作引导火焰的煤油超声速燃烧进行了研究。根据试验测得的壁面静压分布，采用一维简化模型处理与分析数据，得出了不同试验条件下的燃烧效率与总压恢复系数；对超声速燃烧室内的静压分布特点作出了分析；对超声速燃烧室人口处的气流总温，燃料喷射位置，以及燃烧总体当时比对燃烧室内静压分布、燃烧效率与总压恢复系数的影响进行了讨论。