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。     

空间电源功率调节技术综述

介绍了空间电源功率调节装置(PCU)的分流调节器(SR),蓄电池的充电控制器(BCR)、放电控制器(BDR)和主误差放大器(MEA)的原理和技术现状。阐述了顺序开关分流调节(S3R)、混合型调节和顺序开关分流串联调节(S4R)三种基本拓扑的工作原理,并对三者进行了性能比较,认为S4R是目前最先进的调节技术。讨论了功率调节装置模块化、智能化和小型化的发展趋势并分析了大功率的功率调节装置研制难点。     

基于粒子云方法研究地磁场对运动电子束的时空分布影响

空间电荷效应是空间带电粒子分布直接产生的相关效应,对于理解空间辐射环境有着重要意义。为研究地球磁场对空间电荷效应的影响,文章通过数值求解Poisson方程和相对论粒子运动方程,建立粒子云（particle-in-cell, PIC）自洽模型,并构建地球偶极子磁场模型作为内磁层背景磁场（空间分布L值为3～7）。在模型基础上,给出内磁层典型电子束结构（能量0.1～100 keV）的两种初始分布（Uniform和Gaussian分布）,模拟电子束在地磁场影响下的动力学过程。结果表明：电子束结构受地磁场影响出现纵向的整体偏转,并由于自场效应产生了纵向的拉伸和横向的发散;电子束整体的偏转角主要受地磁场强弱以及电子束运动与磁场夹角影响,而拉伸和发散效应则主要受电子束能量等参数所影响。     

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.     

锯齿扁管内沸腾换热试验

建立以等热流密度方式进行试验件加热的沸腾换热试验系统,分别对当量直径为1.28mm和1.59mm锯齿扁管内R134a工质的沸腾换热特性进行研究,试验参数范围:制冷剂质量流率为68.5~305.5kg/(m2·s),工作饱和压力为0.27~0.46 MPa,加热热流密度为9~42kW/m2。试验结果表明:相同结构的通道,当量直径小换热能力更强;热流密度和饱和压力对沸腾换热的影响与一个干度值有关。当干度小于此值时,沸腾换热系数会随着热流密度及饱和压力增大而增大;而当干度大于此值时,沸腾换热系数随着干度增大而急剧下降,热流密度和饱和压力对换热的影响较小;该干度值会随着热流密度或饱和压力增大而逐渐变小。质量流率对沸腾换热的影响与热流密度有关,随着热流密度增大,质量流率的影响趋向大干度区域。通过分析各参数对沸腾换热的影响,建立了一个预测试验工况下微小尺寸锯齿扁管的沸腾换热系数计算经验公式。     

环型与线型聚能装药射流成型机理对比

环型聚能装药药型罩2侧在挤压汇聚形成射流过程中存在不对称性,不能完全套用线型聚能装药射流成型的现有理论。利用DYNA3D软件对相同剖面结构的环型、线型聚能装药射流成型过程进行数值模拟,通过比较分析得出了环型聚能装药形成杵体及射流参数的分布特性,为进一步理论研究及工程应用提供参考。     

基于压电式加速度计的振动测量原理及应用

阐述了利用压电式加速度计、电荷放大器、动态信号分析仪进行振动测量的原理及应用。     

星载蓄电池组软件V/T充电控制技术研究

蓄电池组作为整星的储能部件,其充放电循环寿命是制约整星寿命的重要因素之一。适当的充电控制手段能有效地延缓蓄电池性能的衰降,延长卫星的使用寿命。文章分析了目前基于硬件模拟电路的蓄电池电压/温度（V/T）曲线充电控制技术的特点和局限性,提出了一种采用电源控制计算机软件实现的V/T曲线充电控制方法,其针对蓄电池可能出现的开路...     

CubeSail: A low cost CubeSat based solar sail demonstration mission

CubeSail is a nano-solar sail mission based on the 3U CubeSat standard, which is currently being designed and built at the Surrey Space Centre, University of Surrey. CubeSail will have a total mass of around 3 kg and will deploy a 5 × 5 m sail in low Earth orbit. The primary aim of the mission is to demonstrate the concept of solar sailing and end-of-life de-orbiting using the sail membrane as a drag-sail. The spacecraft will have a compact 3-axis stabilised attitude control system, which uses three magnetic torquers aligned with the spacecraft principle axis as well as a novel two-dimensional translation stage separating the spacecraft bus from the sail. CubeSail’s deployment mechanism consists of four novel booms and four-quadrant sail membranes. The proposed booms are made from tape-spring blades and will deploy the sail membrane from a 2U CubeSat standard structure. This paper presents a systems level overview of the CubeSat mission, focusing on the mission orbit and de-orbiting, in addition to the deployment, attitude control and the satellite bus.     

卫星表面材料物性与电荷积累

卫星表面在地磁亚暴环境下积累电荷的现象是必然的。由于表面间物性的差别,这种积累将是不均衡的,然而一旦建立了电势差,那末表面与表面,表面与构架间就会存在电荷交换,使电势差逐渐趋于减小。文章试图通过物理模型的建立,由此推导出面间电势差变化与表面电势值及表面的电导、电容的关系,从而建立一种明确的数学模型,以利卫星表面充电状态的分析。