Far ultraviolet imaging from the IMAGE spacecraft. 2. Wideband FUV imaging

The Far Ultraviolet Wideband Imaging Camera (WIC) complements the magnetospheric images taken by the IMAGE satellite instruments with simultaneous global maps of the terrestrial aurora. Thus, a primary requirement of WIC is to image the total intensity of the aurora in wavelength regions most representative of the auroral source and least contaminated by dayglow, have sufficient field of view to cover the entire polar region from spacecraft apogee and have resolution that is sufficient to resolve auroras on a scale of 1 to 2 latitude degrees. The instrument is sensitive in the spectral region from 140–190 nm. The WIC is mounted on the rotating IMAGE spacecraft viewing radially outward and has a field of view of 17° in the direction parallel to the spacecraft spin axis. Its field of view is 30° in the direction perpendicular to the spin axis, although only a 17°×17° image of the Earth is recorded. The optics was an all-reflective, inverted Cassegrain Burch camera using concentric optics with a small convex primary and a large concave secondary mirror. The mirrors were coated by a special multi-layer coating, which has low reflectivity in the visible and near UV region. The detector consists of a MCP-intensified CCD. The MCP is curved to accommodate the focal surface of the concentric optics. The phosphor of the image intensifier is deposited on a concave fiberoptic window, which is then coupled to the CCD with a fiberoptic taper. The camera head operates in a fast frame transfer mode with the CCD being read approximately 30 full frames (512×256 pixel) per second with an exposure time of 0.033 s. The image motion due to the satellite spin is minimal during such a short exposure. Each image is electronically distortion corrected using the look up table scheme. An offset is added to each memory address that is proportional to the image shift due to satellite rotation, and the charge signal is digitally summed in memory. On orbit, approximately 300 frames will be added to produce one WIC image in memory. The advantage of the electronic motion compensation and distortion correction is that it is extremely flexible, permitting several kinds of corrections including motions parallel and perpendicular to the predicted axis of rotation. The instrument was calibrated by applying ultraviolet light through a vacuum monochromator and measuring the absolute responsivity of the instrument. To obtain the data for the distortion look up table, the camera was turned through various angles and the input angles corresponding to a pixel matrix were recorded. It was found that the spectral response peaked at 150 nm and fell off in either direction. The equivalent aperture of the camera, including mirror reflectivities and effective photocathode quantum efficiency, is about 0.04 cm². Thus, a 100 Rayleigh aurora is expected to produce 23 equivalent counts per pixel per 10 s exposure at the peak of instrument response.     

Global imaging of O+ from IMAGE/HENA

The magnetospheric O⁺ population in the 52–180 keV range during storms is investigated through the analysis of energetic neutral atom (ENA) images. The images are obtained from the high energy neutral atom (HENA) imager onboard the IMAGE satellite. At each substorm onset following the commencement of a geomagnetic storm the oxygen ENA display ～30 min intense bursts. Only very weak corresponding features in the 60–119 keV hydrogen ENA can be occasionally seen. The dominating fraction of the oxygen ENA emissions are produced when O⁺ ions mirror/precipitate at low altitudes, where the number density of the neutral atmosphere is high. During the storm we observed several bursts of oxygen ENA, but it is still not clear how much the O⁺ content of the ring current increases during the storm main phase. Our observations suggest that the responsible injection mechanism is mass-dependent and scatters the pitch angles. This leads us to favor a non-adiabatic mechanism proposed by (Delcourt, 2002).     

The design features of the GGS wind and polar spacecraft

The Global Geospace Science (GGS) WIND and POLAR spacecraft employ unique configuration and design features driven by the requirements of the science instruments which they host. The WIND and POLAR spacecraft are cylindrically shaped spinners (WIND 20 rpm, POLAR 10 rpm) approximately 2.4 m in diameter and 1.8 m high. Each spacecraft has a pair of lanyard booms, which hold magnetometers, four radial wire antennas and two spin-axis antennas. While satisfying different mission requirements, both share a common basic design. The WIND laboratory contains 8 instruments, designed to optimize measurements of waves, fields and particle distributions. The POLAR laboratory contains 12 instruments, with a similar design emphasis on waves, fields and particle measurements, as well as on auroral imaging. The main difference between the two spacecraft is a despun platform on POLAR which provides a stable environment for the auroral imager instruments. Both laboratories are designed to be launched on Delta II model 7925 launch vehicle and have total masses of approximately 1150 g (WIND) and 1240 kg (POLAR).     

The visible imaging system (VIS) for the polar spacecraft

The Visible Imaging System (VIS) is a set of three low-light-level cameras to be flown on the POLAR spacecraft of the Global Geospace Science (GGS) program which is an element of the International Solar-Terrestrial Physics (ISTP) campaign. Two of these cameras share primary and some secondary optics and are designed to provide images of the nighttime auroral oval at visible wavelengths. A third camera is used to monitor the directions of the fields-of-view of these sensitive auroral cameras with respect to sunlit Earth. The auroral emissions of interest include those from N ₂ ⁺ at 391.4 nm, Oi at 557.7 and 630.0 nm, Hi at 656.3 nm, and Oii at 732.0 nm. The two auroral cameras have different spatial resolutions. These resolutions are about 10 and 20 km from a spacecraft altitude of 8R _e . The time to acquire and telemeter a 256×256-pixel image is about 12 s. The primary scientific objectives of this imaging instrumentation, together with thein-situ observations from the ensemble of ISTP spacecraft, are (1) quantitative assessment of the dissipation of magnetospheric energy into the auroral ionosphere, (2) an instantaneous reference system for thein-situ measurements, (3) development of a substantial model for energy flow within the magnetosphere, (4) investigation of the topology of the magnetosphere, and (5) delineation of the responses of the magnetosphere to substorms and variable solar wind conditions.     

航天器在轨可更换模块机构与结构设计

航天器常在其任务中出现功能失效,造成巨大的损失,而在轨模块更换技术则是利用空间机械臂自主对可接受在轨服务航天器进行故障模块更换、升级、补充消耗品等。通过对在轨可更换模块在轨服务的任务、在轨可更换模块的组件构成,从而得出在轨可更换模块的机构设计方案,进而又对在轨可更换模块进行结构设计,利用 SolidWorks 软件建立该结构的三维模型,实物模型验证了其可行性。     

An approach to forming the design performance of the attitude control system for small spacecraft

The elements for various types of attitude control systems used in a number of small spacecraft are considered. An approach for assessment of such system effectiveness based on design requirements for spacecraft purpose and restriction in accuracy, mass and energy is proposed.     

Concerning the interpretation of the ultraviolet radiation from B stars

Measurements of the shape of the ultraviolet spectrum from B stars are compared with the theoretical spectra predicted from a homogeneous series of eight model atmospheres which are known to be close to a state of radiative equilibrium and to give a good representation of the ordinarily observed spectral region. The broad-band photometer measurements of Byram, Chubb, and Friedman in the region 1314 indicate that the stars become brighter in the ultraviolet as their temperature increases. The theoretical spectra reproduce this trend. However, the theoretical spectra are about three times as bright at 1314 relative to their brightness at 5560 as is observed.The spectral observations at 50Å resolution of Stecher and Milligan of six absorption-line stars are compared in detail with theoretical spectra. The observed shape of the spectrum is reproduced well by the models from 2600 to longer wavelengths. At wavelengths shorter than 2600 Å, the observed fluxes from B stars are less than the predicted fluxes. At 2000 the deficiency is between a factor two and a factor four. The spectrum of Canis Majoris is observed to have a different shape from that found for four other early-type stars. In the case of Canis Majoris the deficiency at 2000 is about a factor 13.The proper manner in which to compare theory and observation is discussed and some astrophysical terminology is explained. Theoretical fluxes, , are given in Table 1 for eight early B type model atmospheres at wavelengths between the Lyman limit and 6251. These fluxes have been computed without consideration of the opacity due to line blanketing. It is shown that line blanketing can probably account for the differences noted between predicted and observed ultra-violet spectra of B stars. It is not necessary at present to invoke unusual sources of opacity in the stellar atmosphere or in the space between the star and the earth in order to explain the observations. Spectra of B stars in the 2000 region at sufficient resolution to show the line spectrum would clarify the problem.     

飞机研制的新要求谈高强度辐射场(HIRF)防护

与自然界产生的闪电不同,高强度电磁辐射是由人类活动造成的电磁环境问题,其频带宽(10千赫～40吉赫),作用时间长(与闪电的作用时间相比)。高强度电磁辐射、闪电与电磁兼容等电磁环境问题(统称 E3问题),已成为影响飞机安全的重要因素。因此,在飞机研制中,应采取措施对飞机的电子和电气系统进行保护,以免对飞行安全带来不利影响。     

从航空武器装备维修体制变化看ATE的发展趋势

以装备维修体制变化为背景,阐述了自动测试设备(ATE)在装备三级维修中的应用,研究了两级维修体制下的各级测试需求,结合国外军队ATE的近期研究状况,分析了其最新趋势,从而为我军ATE的研制提供了借鉴.     

从总体设计角度透视高超声速飞行器边界层转捩问题

边界层转捩对飞行器总体性能影响很大,按照弹道式再入、再入机动、高超声速滑翔、高超声速巡航四类飞行器进行分类,与边界层转捩相关的典型问题可归结为气动力、气动热及掺混效率三类,相应带来飞行稳定性与配平能力、落点散布、防热风险、飞行器减重、推进系统优化等问题.针对边界层转捩控制问题,从总体设计方面可采取弹道设计、翼载荷控制、...     

由美军无人机系统的发展引发的思考

简要介绍了目前美军无人机的研制发展和装备情况，着重分析了当前美军无人机发展的三大特点，即作战区域覆盖全球、作战任务类型繁多，大量新技术的应用以及强调无人机的能力和智能化程度。并对我国无人机的发展提出了系统规划无人机平台体系，改研和新研协调发展以及重视反无人机战术技术研究的建议。     

Plasma density measurements from the GEOS-1 relaxation sounder

The relaxation sounder uses the characteristics of the propagation of radiowaves to sound the plasma surrounding the spacecraft. It determines, in particular, the plasma frequency, which gives the electron density.We have now measurements over the whole dayside of the magnetosphere, from the evening to the night sectors.The behaviour of the plasma resonance depends on local time, the nightime echoes being generally weaker.Density measurements thus obtained are shown and discussed in the context of what is presently known about the plasma distribution in the magnetosphere. In particular, the density around apogee is studied as a function of magnetic activity. On the dayside, it appears to vary between a few and a few tens of electrons per cubic centimeter. The evolution of the density profile for several consecutive days is studied and interpreted tracing back the drift of the particles.     

由“钻石体系”看日本产业竞争力

迈克尔·波特按照“钻石体系”四要素(生产要素,需求条件,相关与支持性产业和企业结构、企业战略、同业竞争)以及政府和机遇等方面分析日本产业竞争力,从其分析日本产业成功的原因中得出提升中国产业竞争力的启示。     

英、法标准化机构及其运行机制对我们的启示

介绍了英国标准学会 (BSI)和法国航空航天标准化局 (BNAE)的性质、经费来源和运作概况 ,以及欧洲航空领域标准化的发展趋向。兼谈了我们从英、法标准化机构的运作模式和发展趋势中得到的启示。     

First results from the six-axis electron spectrometer on ISEE-1

A survey, using results from the first 25 orbits of ISEE-1, has been made of some aspects of electrons in the dawn magnetosheath. There are indications that the flow of plasma is not uniformly turbulent over this region. The electron heat flux is observed to be directed away from the shock and to have an average value of about twice the interplanetary heat flux. Many magnetopause crossings were observed and usually resemble abrupt transitions from one well-defined plasma state to another. The ejection of plasma from flux tubes converted up against the magnetopause is observed for about half the time, and its thickness and dependence on the solar wind mach number agree with theoretical predictions. A full traversal of the whole forward hemisphere of the magnetosheath is required to fully confirm these deductions.     

高校创业教育系统的构建——基于协同学视角

协同创新作为一种全新的教育理念,为高校教育教学改革,尤其是创业教育指明了方向。基于协同学理论和大学生创业教育体系相互关系,分析了高校创业教育中存在的突出问题,从理念、内容、组织和政策四个层面构建了创业教育的系统模型。