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.     

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。     

机电作动系统发展

 机电作动系统是通过控制电动机或电器的运行直接或间接地控制负载的运动，实现控制目标的位置伺服控制的一类系统的总称。针对飞行器用机电作动系统，概述了其应用概况、结构的演化过程、关键技术的发展过程，并就机电作动系统的发展动态做了介绍。在此基础上，提出了飞行器用机电作动系统的研究和发展的一些建议。     

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。     

The Plasma Environment of Comet 67P/Churyumov-Gerasimenko Throughout the Rosetta Main Mission

The plasma environment of comet 67P/Churyumov-Gerasimenko, the Rosetta mission target comet, is explored over a range of heliocentric distances throughout the mission: 3.25 AU (Rosetta instruments on), 2.7 AU (Lander down), 2.0 AU, and 1.3 AU (perihelion). Because of the large range of gas production rates, we have used both a fluid-based magnetohydrodynamic (MHD) model as well as a semi-kinetic hybrid particle model to study the plasma distribution. We describe the variation in plasma environs over the mission as well as the differences between the two modeling approaches under different conditions. In addition, we present results from a field aligned, two-stream transport electron model of the suprathermal electron flux when the comet is near perihelion.     

Relationship Between Substorm Auroras and Processes in the Near-Earth Magnetotail

Although the auroral substorm has been long regarded as a manifestation of the magnetospheric substorm, a direct relation of active auroras to certain magnetospheric processes is still debatable. To investigate the relationship, we combine the data of the UV imager onboard the Polar satellite with plasma and magnetic field measurements by the Geotail spacecraft. The poleward edge of the auroral bulge, as determined from the images obtained at the LHBL passband, is found to be conjugated with the region where the oppositely directed fast plasma flows observed in the near-Earth plasma sheet during substorms are generated. We conclude that the auroras forming the bulge are due to the near-Earth reconnection process. This implies that the magnetic flux through the auroral bulge is equal to the flux dissipated in the magnetotail during the substorm. Comparison of the magnetic flux through the auroral bulge with the magnetic flux accumulated in the tail lobe during the growth phase shows that these parameters have the comparable values. This is a clear evidence of the loading–unloading scheme of substorm development. It is shown that the area of the auroral bulge developing during substorm is proportional to the total (magnetic plus plasma) pressure decrease in the magnetotail. These findings stress the importance of auroral bulge observations for monitoring of substorm intensity in terms of the magnetic flux and energy dissipation.     

Type II Solar Radio Bursts: Theory and Space Weather Implications

Recent data and theory for type II solar radio bursts are reviewed, focusing on a recent analytic quantitative theory for interplanetary type II bursts. The theory addresses electron reflection and acceleration at the type II shock, formation of electron beams in the foreshock, and generation of Langmuir waves and the type II radiation there. The theory's predictions as functions of the shock and plasma parameters are summarized and discussed in terms of space weather events. The theory is consistent with available data, has explanations for radio-loud/quiet coronal mass ejections (CMEs) and why type IIs are bursty, and can account for empirical correlations between type IIs, CMEs, and interplanetary disturbances. This revised version was published online in August 2006 with corrections to the Cover Date.     

光纤表面等离子体波传感器用于固化监测的研究(英文)

光纤表面等离子体波传感器在理论上具有较高的研究价值 ,并且因为结构简单、灵敏度高等特点在工程上得到广泛应用。使用光纤表面等离子体波来测试折射率 ,方法简单、灵敏。本文介绍了利用光纤表面等离子体波传感器使用这种方法对环氧树脂复合材料进行固化监测。文中对不同折射率的溶液进行了折射率测试的研究 ,并设计了一种用于折射率测量的性能稳定、操作方便的光纤传感探头及整套的测试系统 ,用以对固化过程中环氧树脂在不同阶段的折射率变化进行实测。测试结果表明 ,该系统工作稳定、可靠 ,测试结果符合实际情况