Asymmetries in Mars' Exosphere

Observations and simulations show that Mars' atmosphere has large seasonal variations. Total atmospheric density can have an order of magnitude latitudinal variation at exobase heights. By numerical simulations we show that these latitude variations in exobase parameters induce asymmetries in the hydrogen exosphere that propagate to large distances from the planet. We show that these asymmetries in the exosphere produce asymmetries in the fluxes of energetic neutral atoms (ENAs) and soft X-rays produced by charge exchange between the solar wind and exospheric hydrogen. This could be an explanation for asymmetries that have been observed in ENA and X-ray fluxes at Mars.     

Global Response of Martian Plasma Environment to an Interplanetary Structure: From Ena and Plasma Observations at Mars

As a part of the global plasma environment study of Mars and its response to the solar wind, we have analyzed a peculiar case of the subsolar energetic neutral atom (ENA) jet observed on June 7, 2004 by the Neutral Particle Detector (NPD) on board the Mars Express satellite. The “subsolar ENA jet” is generated by the interaction between the solar wind and the Martian exosphere, and is one of the most intense sources of ENA flux observed in the vicinity of Mars. On June 7, 2004 (orbit 485 of Mars Express), the NPD observed a very intense subsolar ENA jet, which then abruptly decreased within ∼10 sec followed by quasi-periodic (∼1 min) flux variations. Simultaneously, the plasma sensors detected a solar wind structure, which was most likely an interplanetary shock surface. The abrupt decrease of the ENA flux and the quasi-periodic flux variations can be understood in the framework of the global response of the Martian plasma obstacle to the interplanetary shock. The generation region of the subsolar ENA jet was pushed towards the planet by the interplanetary shock; and therefore, Mars Express went out of the ENA jet region. Associated global vibrations of the Martian plasma obstacle may have been the cause of the quasi-periodic flux variations of the ENA flux at the spacecraft location.     

小波分析和人工神经网络在金属超声无损检测缺陷分类中的应用

基于金属超声检测中的缺陷脉冲回波为非稳态信号的特点，对高温合金材料超声检测信号的小波变换进行了特征分析，提取了各级小波分解信号的能量分布特征，最后将这些特征输入人工神经网络进行训练和分类，实验表明，这种方法具有良好效果。     

中性浮力微重力环境模拟技术

我国载人试验飞船发射成功后,对载人航天用的大型中性浮力模拟器的需求越来越迫切。文章通过对国外中性浮力模拟试验和设备情况的介绍,归纳出该类设备主要的5类应用,并提出对我国大型中性浮力模拟器设备的总体设想。     

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.     

室火轰燃的大涡模拟

采用一套修正的适用于低马赫数浮力流的N-S方程组来描述火灾场,运用Smagorinsky亚格子模型的大涡模拟方法对室内池火的轰燃发展过程进行了数值模拟,把模拟与实验结果进行了对比和分析。结果表明,该方法能较好地预测轰燃。同时模拟结果显示火焰区向房间后部偏转稍大,近壁处温度预测的误差大一些,随着亚格子模型的不断完善和计算能力的提高,用该技术来预测轰燃现象会更加准确。     

中性稳定技术在综合火力/飞行控制系统中的应用

火力／飞行综合控制(Integrated fire／flight control，IFFC)系统要求对飞机飞行姿态的控制应具有精确性和快速性，但提高姿态跟踪精度受到自然飞机惯性动力学的限制。本文提出飞机中性稳定技术应用于综合火力／飞行控制系统，给出了中性稳定飞机结构图和动力学模型。利用后缘襟副翼偏转所产生的直接力效果，在一定的控制律制约下，去抵消迎角扰动所产生的气动效果，使飞机不再出现静稳定力矩，达到中性稳定。采用中性稳定技术的综合火力／飞行控制系统有效地加速了飞机在攻击区的姿态跟踪过程，并实现了姿态控制过程中航迹基本不变的机身瞄准模态控制要求，提高了火控精度和命中概率。仿真结果表明，中性稳定综合火力／飞行控制系统具有良好的控制效果和应用前景。     

剩余浮力对系留气球静平衡特性的影响分析

在进行系留气球总体方案设计时,剩余浮力的选择直接影响到系留气球气囊和副气囊体积等参数的设计,剩余浮力选择不当将造成研制成本的增加或静平衡特性指标无法实现。因此,对同一系留气球不同剩余浮力,及两种不同体积的系留气球在相同剩余浮力时的静平衡特性进行计算与对比分析。结果表明:对同一体积的系留气球,剩余浮力对系留气球俯仰角、高度损失和水平漂移量影响较大,且剩余浮力越大,其俯仰角、高度损失和水平漂移量越小;随着系留气球体积的增大,剩余浮力对系留气球高度损失和水平漂移量的影响将逐渐减小。     

基于中性层偏移的Z型材滚弯成形回弹预测

以提高大截面Z型材四轴滚弯成形精度为目的，通过综合考虑材料属性、几何特征和成形半径等因素对回弹的影响，建立了引入中性层偏移的大截面Z型材弯曲回弹解析模型，研究了7075-O和7475-O铝合金Z型材在不同滚弯成形半径下的回弹规律，并进行滚弯成形实验验证。结果表明，与忽略中性层偏移影响的型材回弹预测经验模型相比，基于中性层偏移的回弹预测模型能够准确预测大截面Z型材的回弹量，在相同的曲率半径下，预测回弹变形的最大相对误差从11.681%减小到3.347%。     

Energetic Hydrogen and Oxygen Atoms Observed on the Nightside of Mars

We present measurements of energetic hydrogen and oxygen atoms (ENAs) on the nightside of Mars detected by the neutral particle detector (NPD) of ASPERA-3 on Mars Express. We focus on the observations for which the field-of-view of NPD was directed at the nightside of Mars or at the region around the limb, thus monitoring the flow of ENAs towards the nightside of the planet. We derive energy spectra and total fluxes, and have compiled maps of hydrogen ENA outflow. The hydrogen ENA intensities reach 10⁵ cm⁻² sr⁻¹ s⁻¹, but no oxygen ENA signals above the detection threshold of 10⁴ cm⁻² sr⁻¹ s⁻¹ are observed. These intensities are considerably lower than most theoretical predictions. We explain the discrepancy as due to an overestimation of the charge-exchange processes in the models for which too high an exospheric density was assumed. Recent UV limb emission measurements (Galli et al., this issue) point to a hydrogen exobase density of 10¹⁰ m⁻³ and a very hot hydrogen component, whereas the models were based on a hydrogen exobase density of 10¹² m⁻³ and a temperature of 200 K predicted by Krasnopolsky and Gladstone (1996). Finally, we estimate the global atmospheric loss rate of hydrogen and oxygen due to the production of ENAs.