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.     

热防护系统高温纤维隔热毡传热及有效热导率分析

针对重复使用运载器热防护系统纤维隔热毡内部导热和辐射的耦合换热问题进行了分析,应用有限差分法建立了纤维隔热毡的数值分析模型.通过数值求解传热方程,计算了稳态的有效热导率.计算结果表明辐射和气体传导是纤维隔热毡内的主要传热方式,辐射作用随压力和试样密度的增加而降低,在试样温度高的一侧辐射是主要的传热方式,而在温度低的一侧气体传导为主要的传热方式;试样的有效热导率随纤维的平均直径、压力和温差的增加而增加,随试样密度的增加而降低.本文的计算结果与文献中的实验结果吻合较好,可以为纤维隔热毡及热防护系统的优化设计提供理论参考.     

基于VXI总线的检测软件设计

基于VXI总线和虚拟仪器技术，研制开发了用于外场的模拟式电子控制器检测软件，并对软件开发的过程和要求进行了分析，重点解决了程序设计中的需求分析和模块化设计问题。     

Variations of the magnetic fields in large solar flares

We present preliminary results from high resolution observations obtained with the Michelson Doppler Imager (MDI) instrument on the SOHO of two large solar flares of 14 July 2000 and 24 November 2000. We show that rapid variations of the line-of-sight magnetic field occured on a time scale of a few minutes during the flare explosions. The reversibility/irreversibility of the magnetic field of both active regions is a very good tool for understanding how the magnetic energy is released in these flares. The observed sharp increase of the magnetic energy density at the time of maximum of the solar flare could involve an unknown component which deposited supplementary energy into the system. This revised version was published online in August 2006 with corrections to the Cover Date.     

三轴稳定卫星无陀螺姿态确定算法研究

针对三轴稳定卫星进行了正常飞行模式下无陀螺姿态确定算法研究，采用磁强计、地球敏感器和太阳敏感器组合获得姿态数据，利用四元数法和高斯－马尔可夫过程建立了姿态确定估计器算法模型。通过数学仿真证明，此姿态确定算法能够对星体姿态进行较精确的估计或校正，满足卫星控制精度要求。     

磁制动对地壳板块运动影响的理论分析与实证研究

太阳和木星的自转是不均匀的，纬度愈高，自转愈慢。据此，作者推测液态外地核的自转，也存在类似的不均匀性，而这种不均匀自转将对地壳板块运动产生影响。利用磁流体力学理论，阐明这类星球自转的不均匀性，是磁制动的不均匀性引起的。研究了磁制动对地壳板块运动影响的途径及表现方式，并举出实例证明这些表现方式的确存在，从而证明磁制动是影响地壳板块运动的一个极为重要的因素。     

应用声发射技术实时监测某型机防扭支架疲劳试验裂纹

随着声发射技术的发展,声发射技术在工程无损检测上的运用日益广泛。本文对声发射技术的应用现状、基本理论及在直升机某型机防扭支架疲劳试验裂纹监测中的应用进行了介绍。希望通过应用声发射技术,能及时捕捉疲劳裂纹形成和扩展的过程,给判定疲劳试验件是否破坏带来更准确、客观的依据,从而能为直升机动部件和结构件的准确定寿提供一种科学的辅助手段。     

EXPERIMENTAL RESEARCH ON STRESS INTENSITY FACTOR K_Ⅲ FOR 3-D CRACK BY CAUSTICS

ＥＸＰＥＲＩＭＥＮＴＡＬＲＥＳＥＡＲＣＨＯＮＳＴＲＥＳＳＩＮＴＥＮＳＩＴＹＦＡＣＴＯＲＫⅢＦＯＲ３┐ＤＣＲＡＣＫＢＹＣＡＵＳＴＩＣＳＷｕＤａｆａｎｇ，ＧａｏＺｈｅｎｔｏｎｇ（ＩｎｓｔｉｔｕｔｅｏｆＳｏｌｉｄＭｅｃｈａｎｉｃｓ，ＢｅｉｊｉｎｇＵｎｉｖｅ...     

从PCI-A429芯片谈内核的设计及集成

以自行研制的PCI-A429芯片为例,讨论了内核设计以及系统集成中内核互连的问题。主要介绍了程控配置和自适应方式的两种ARINC429接收模块内核和PCI内核的设计。还分析了内核之间互连的多种控制接口和数据接口。     

改进的P型迭代学习控制算法

针对多输入多输出的定常线性系统的迭代学习控制问题, 给出改进的P型迭代学习控制算法, 该算法中利用最新算出的控制分量代替旧的控制分量, 这样可以加快控制输入的收敛速度, 利用该算法进行学习控制, 使系统的实际输出以更快的速度收敛于系统的理想输出.