镉镍电池在武器回收系统中的应用探讨

文章对镉镍电池在武器回收系统中的应用进行了探讨 ,得到了在武器回收系统中可以用镉镍充电电池取代银锌蓄电池的结论     

翼柱型装药发动机点火升压过程计算

利用实验获得的翼槽内火焰传播规律经验公式,在Ｐ（ｔ）模型的基础上,建立了翼柱型发动机的点火升压计算模型。计算结果与实测数据吻合较好。同时就点火器流量、推进剂燃速、喷管堵盖打开压强等设计参数对发动机点火升压过程的影响进行了分析。     

固体火箭发动机点火药量的计算

通过对点火过程及数学模型的描述，以气体状态方程计算点火药量的公式为基础，提出了一个新的点火药量计算经验公式，并讨论了公式的应用情况和使用范围。     

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.     

微型固体火箭发动机用短点火延迟点火器研究

短的点火延迟期对某些微型固体火箭发动机尤为重要。文中引用固相点火理论，在诸多向推进剂表面供热的方式中，着重分析了起重要作用的对流换热，认为提高点火燃气的流速能明显地提高点火燃气对推进剂表面的热交换率，使推进剂表面很快达到发火温度，在微型固体火箭发动机的短点火延迟点火器设计中应用了这一理论，并获得了理想的效果。     

变几何喉道对超燃冲压发动机点火与燃烧性能的影响

1引言超燃冲压发动机能高速飞行且能利用空气中的氧气作氧化剂,增加了有效载荷,因而备受重视,但它需要在较高的飞行马赫数下才能工作,因此受到较大的限制。由于双模态超燃冲压发动机可以将工作飞行马赫数下限降低至Ma=3,发动机在飞行马赫数Ma=3~6时以亚燃冲压模态工作,在马赫数     

提高WP－11发动机起动高度的研究与实施

研究了ＷＰ－１１发动机点火高度从４０００ｍ提高到８０００ｍ的某些问题。详细讨论了点火高度的理论基础，并为ＷＰ－１１研制了一种可用的空中补氧点火装置，扩大了ＷＰ－１１发动机的使用范围。带着空中补氧点火装置的ＷＰ－１１发动机成功完成了高空舱试验和Ｙ－８飞机带飞实验。     

固体推进剂等离子体点火研究

为了研究等离子体对固体推进剂点火性能的影响，分别对双基药和硝胺药等两种固体推进剂，进行了等离子体点火实验。实验装置包括等离子体源、热电偶丝和动态信号分析仪。通过实验，获得了两种固体推进剂在不同的等离子体能量输入的条件下，其表面温度随时间变化的曲线。与常规点火数据相比，固体推进剂的等离子体点火延迟时间明显缩短。不同类型的固体推进剂，在相同的等离子体能量输入条件下，其点火性能不同；同一种类型的固体推进剂，在不同的等离子体能量输入条件下，其点火性能也不一样。     

点火能量等因素对脉冲爆震室压的影响实验

以汽油／空气两相混气为可爆混合物，采用汽油机点火和半导体高能点火系统，实验研究了不同点火频率对脉冲爆震室中不同位置脉冲爆震波压力的影响，结果发现，充满度大，产生的紊流强度大，有利于爆震波的形成；在大多数情况下，用低能量（50mJ）的点火系统点火时，点火频率大于实际产生的爆震频率；用高能（IJ）点火系统时，可缩短烯向爆震转变（DDT）的距离，易产生爆震，所得爆震波的峰值压力明显增大，所得结果可为脉冲爆震发动机的设计、爆震点火系统选型提供重要参考。     

固体火箭发动机特征间隙分析

为了分析大长径比固体火箭发动机点火瞬态过程性能散布的主要原因，引入特征间隙概念，分析了其性质，并验证其适用性，将其作为设计准则，分析了两台发动机点火瞬态过程，认为大长径比发动机点火瞬态过程性能散布主要原因不是加工精度，而是点火装置性能散布，并用数值计算验证了这一结论。