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.     

可重复使用热防护材料应用与研究进展

可重复使用热防护系统是为高速重复使用飞行器而发展的关键性技术,涵盖了地球大气环境及非地球大气环境下的弹道式再入、高马赫数巡航等应用场景。根据现有高马赫数飞行器热防护现状,对高马赫数飞行器的主要热防护系统类型、特点和使用场景进行了简要介绍。在此基础上,结合国外里程碑式可重复使用飞行器（X-15、SR-71、航天飞机、X-33、X-37B、Spaceliner等）,梳理了可重复使用热防护材料的应用与研究进展,论述了代表性可重复使用热防护材料的发展、性能、研制进度、特点及应用前景。对国外在可重复使用热防护材料研制中的设计及发展思路,以及所存在的主要问题进行了总结归纳,为可重复使用热防护材料未来的发展提供了思路。     

MA 及原位-热压合成TiC/ Ti5 Si3 复合材料

以Ti粉、Si粉和C粉为原料,利用高能球磨及热压工艺合成了TiC/Ti5Si3陶瓷复合材料。研究了工艺条件尤其是热压温度对合成产物相组成及微观结构的影响,并结合DSC、XRD和SEM对反应合成机理进行探讨。结果表明:通过优化合成工艺,高能球磨12 h,热压温度1 400℃时,烧结6 h得到了高纯度的TiC/Ti5Si3陶瓷复合材料;合成过程为:反应开始时发生Ti+C■TiC,反应ΔG=-167.72 kJ/mol。2 h时发生5TiC+8Si■Ti5Si3+5SiC,反应ΔG=-62.12 kJ/mol,当6 h时发生3SiC+8Ti■Ti5Si3+3TiC,反应ΔG=-697.8 kJ/mol。显微结构表明:TiC/Ti5Si3复合材料的合成过程伴随Si熔融,该材料以TiC-Si-Ti5Si3形式相结合,其中Si为黏结剂。     

齿冠形收敛喷管模型气动和红外辐射特性数值研究

针对齿冠形收敛喷管的气动和红外辐射特性进行了数值计算,并与常规收敛喷管进行了对比.在本文研究范围内的结果表明:①齿冠形收敛喷管的推力损失大于常规收敛喷管;②齿冠形尾缘引射外界大气与主流掺混的能力强于常规收敛喷管,核心区长度得到有效衰减;③齿冠形喷管的热喷流3～5μm红外辐射强度在侧向相对常规收敛喷管的衰减量在15%左右,尾缘内倾角对于尾喷流红外辐射强度衰减的影响甚微;④齿冠内倾时,尾向处能遮挡喷管内部热部件.      

着陆襟翼打开状态下抓斗式反推装置 三维流动数值模拟

基于求解三维Reynolds-averaged Navier-Stokes方程,数值模拟了着陆襟翼打开状态下抓斗式反推装置工作时流场分布特性.网格采用非结构化四面体与六面体混合分区生成技术,湍流模型选用Spalart-Allmaras模型.结果表明,在计算滑跑速度范围内,反向排气流不会被进气道重新吸入;高温反向排气流会冲击到飞机吊挂及部分机翼,需引起注意;随着滑跑速度的降低,反向排气流侧向影响范围急剧增大,若机翼后掠角较大,则反向排气流容易被相邻发动机再次吸入,引起进气畸变;当滑跑速度降低到34m/s时,反向流开始吹向地面,可能会卷起地面颗粒物并且被进气道吸入;随着滑跑速度的降低,反推力减小.      

新型超高强Al-Zn-Mg-Cu铝合金热压缩变形的流变应力行为

采用热力模拟试验方法进行热压缩变形试验,研究了一种新型Al-Zn-Mg-Cu合金在变形温度为300～450℃,应变速率为0.001～1s-1,压缩变形程度为50%条件下的流变应力行为.结果表明,变形温度和应变速率对合金流变应力的大小影响显著,流变应力随变形温度的升高而降低,随应变速率的提高而增大.采用统计回归方法建立了...     

磁激等离子体超声速气流的瞬态加速系统及其实验研究

研制了基于激波风洞的热电离系统,设计了马赫数Ma=1.5的喷管和分段法拉第型实验段,并选用了合理的磁场及电场方案。采用氦气驱动氩气模式,通过在激波管低压段注入电离种子K₂CO₃粉末实现气流的热电离;压缩后的高温氩气启动喷管,以瞬态超声速导电流体形式通过实验段。实验结果表明:当激波管高压段压力为1.1 MPa、低压段压力为500 Pa时,喷管出口的超声速导电气流温度约为4 185.91 K,压力约为0.037 MPa;当电容电压为400 V、磁感应强度为1.0 T时,由实验段中间位置电极的放电特性可以估算出气流电导率约为78.1 S/m,单对电极输入功率约为9.46 kW;用感应电压法对加速效果进行初步评估,出口气流速度增加了29.3%,电效率为26.1%。     

粉末耐热钛合金组织性能及成形技术

采用热等静压技术及旋转电极粉,采用预合金粉粉末冶金工艺开展了粉末耐热钛合金TC11(Ti-6.5AJ-3.5Mo-1.5Zr-0.3Si)制备技术研究,研制出了全致密粉末TC11合金,通过热处理工艺研究优化粉末TC11材料的组织和性能.利用光学显微镜,对其组织进行了分析,用SEM观察了旋转电极粉末形貌,对室温及高温(550℃)拉伸性能及弹性模量等进行了测试分析.粉末TC11合金的组织和性能与同批次TC11锻棒材料进行了对比研究.利用特殊模具成形,开展了粉末TC11构件近净成形技术的研究,实现了整体大尺寸、带网格加强筋的薄壁粉末TC11合金航天飞行器舱体件近净成形,且未检测出内部缺陷.研究结果表明,粉末TC11合金具有与锻造材料相当的拉伸性能,而弹性模量更优,其金相组织均匀细致,形成了网篮组织,并有围绕其分布的等轴α.粉末TC11合金及合适的近净成形技术可在高性价比、高可靠性的轻质耐热航天飞行器构件制备中得到应用.     

交流阻抗谱法评价热障涂层的热腐蚀行为(英文)

本文利用交流阻抗这种无损检测的方法研究了热障涂层在质量分数为25%NaCl+75%Na2SO4混合盐体系中的热腐蚀行为。实验结果显示,热腐蚀条件下,在陶瓷层和粘结层界面处形成TGO层为混合氧化物层,成分为Cr2O3、(Ni,Co)(Cr,Al)2O4和NiO,其厚度增长符合抛物线规律。热障涂层在110个循环腐蚀之前时,TGO层的电阻值随其厚度的增加而增加;110个循环后,虽然TGO层的厚度还是在增加,但由于TGO层孔隙的增多而导致其电阻值有所下降。陶瓷层的电阻值随着陶瓷层中裂纹的萌生和扩展而不断增大。等效电路中得到的参数可以用来表征热障涂层的失效行为。     

亚微米晶NiAl-Al2O3复合材料的制备及其烧结-锻造短流程成形

以Ni粉和Al粉为原料,通过机械合金化和真空热压烧结制备了高致密的NiAl-5％Al2O3(体积分数,下同)复合材料,并利用烧结-锻造技术制成了该材料的前缘模拟件.机械球磨后,粉末颗粒充分细化,Ni和Al发生原位反应,并最终生成NiAl-5％Al2O3复合材料粉末.经1300℃真空热压烧结,获得致密的NiAl-Al2O...