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.     

喷气吹气襟翼对翼型气动性能影响研究

用雷诺平均N-S方程模拟方法对翼型上下表面局部增加喷流和吹气的增升效果进行计算分析,内容包括改变喷流压比,喷流角度,舵面状态和吹气位置,以此研究吹气襟翼和喷气襟翼对翼型气动性能的影响规律.模拟结果表明:喷气增升主要通过上下翼面压力分布实现的.在一定范围内升力随喷流的压力比升高而升高;上翼面吹气可以推迟上翼面分离且吹气位置前移推迟分离效果更加明显.     

小功率电弧喷射发动机的数值计算

为详细了解电弧喷射发动机内部工作过程和相关工作参数对其性能的影响，参照实验用发动机的工作参数建立了模型，数值模拟了电弧喷射发动机工作通道内流场和电磁场。利用NND格式求解耦合电磁源项N－S方程，Gauss-Seidel迭代加超松驰方法求解椭圆型电磁场方程，计算得到的发动机工作通道内流场、电磁场结构，与实验数据进行了对比。结果表明，对同一结构尺寸的发动机，随推进剂流量变化，发动机性能存在最佳值；在一定流量范围内，实验数据和计算结果相符。     

冷等离子体处理对碳纤维缝编织物/环氧复合材料界面性能的影响

采用冷等离子体对碳纤维缝编织物进行表面处理 ,并采用XRD对处理前后的碳纤维表面结构进行了分析 ,研究了冷等离子体处理对浸润性以及碳纤维缝编织物 /环氧复合材料的层间剪切强度的影响。实验结果表明 ,冷等离子体处理提高了碳纤维表面活性、浸润性 ,从而改善了碳纤维缝编织物 /环氧复合材料的界面粘结性能 ,进而改善了复合材料的界面性能。     

热处理对大气等离子喷涂纳米结构YSZ热障涂层晶粒长大的影响

采用大气等离子喷涂制备了纳米结构氧化钇稳定的氧化锆热障涂层。运用SEM ,TEM和XRD等方法研究了涂层和原料粉末的微观结构和相组成。结果表明 ,喷涂过程中平均晶粒大小由4 0nm变为 6 7nm ,涂层主要由亚稳四方相组成。涂层热处理结果显示 ,90 0℃以下晶粒长大速度缓慢 ,然而 1 0 0 0℃以上晶粒长大速度迅速增加 ,而且出现较多的单斜相     

相邻激励器合成射流流场数值模拟及机理研究

建立了将合成射流激励器腔体、出口喉道、外部流场作为单连域计算处理的吹／吸型边界模型。在此基础上,对不同相位差、不同振幅、不同频率的相邻激励器相互作用形成的合成射流流场进行了数值分析。计算结果表明：相邻激励器工作时的相位差、振幅不同、驱动频率不同对其形成的合成射流流场有很大影响,合成射流不再对称分布,流动将发生偏转。其机理是由于两激励器吸入和排出流体流动不同(不同相、不同幅值、不同频率),使得两列旋涡对不对称,因此在两列旋涡对之间存在涡量强度不同和压强梯度,从而引起旋涡对向低压侧和强涡量区偏转。     

超声速主流中横向喷流场的激波—旋涡结构的数值模拟

本文利用NND格式,通过求解NS方程,对二维超声速主流中横向喷流干扰流场进行了数值模拟,计算清楚地给出了激波结构、回流区和混合层。本文计算得到的激波结构和实验相当一致。最有兴趣的是由于喷流的干扰,主流在喷口前发生主涡分叉,观察到三个流向旋转涡和两个反流向旋转涡;在喷口后的背风区,存在具有低压和回流区的尾迹。     

粘性气体中粘性液体射流分裂与雾化机理研究

采用线性稳定性分析的方法对粘性气体中的粘性液体射流的分裂与雾化机理进行了分析,数值计算表明:液体射流分裂与雾化过程中存在一临界气体韦伯数We2c=1,We2＜We2c对应的是射流分裂过程,We2＞We2c对应的是射流雾化过程,射流分裂过程和雾化过程的机理有所不同.当We2＜1时,We2对射流分裂过程具有稳定性的作用;当We2＞1时,We2对射流雾化过程起着不稳定性的作用.液体Reynolds数Re1在整个射流过程中始终起着不稳定性的作用,气体Reynolds数Re2的作用却相反.气液密度比Q,即气动力在整个射流分裂与雾化过程中始终起着不稳定性的作用.     

电弧加热发动机温度和速度的测量

本文着重介绍光谱辐射法、激光诱导荧光法、静电探针法等接触式和非接触式测量技术在电弧加热发动机 (Arcjet)参数测量中的应用。讨论了电子温度、重粒子温度、羽流速度等参数的测量 ,并对一些结果进行了分析与论证 ,指出非热力学平衡态下不同的测量技术测量的是不同的温度指标。从测量技术的发展来看 ,激光测量技术将成为参数测量的主导技术。     

加力燃烧室壁温测量试验研究

加力燃烧室燃烧段的壁温对飞机和发动机的安全关系重大,单靠数值计算是很不够的,目前主要靠测试取得。燃烧段通常是双层壁,加风罩则为三层。本文介绍了内外壁和风罩的温度测量方法及其试验研究。该方法对加力燃烧室的研制具有重要意义,无论是对于新机还是批生产发动机都有重要的参考价值。