史密森天文物理观测台研制的冷氢激射器及有关装置

低温冷却激射器为测量频率偏移和存储壁涂敷材料的弛豫特性创造了有利条件。这种涂敷材料是从常态变为气态物质而被冻结在存储壁上的。我们对FEP—120聚四氟乙烯在77K至48K之间的原始测试结果作了报道,并把这些测量结果和法国de Saintfuscien在372K至77K之间的测试数据进行了比较。对激射器的某些设计性能作了说明。低溫激射器的氢分离器,完全密封在真空环境中,其温度77k。本文还介绍了在真空中工作的分离器和其它一些装置。这些装置已在常温激射器中被采用并进行了测试。它们既适合于太空环境又适合于在地面使用。     

Input Parameters for Models of Energetic Electrons Fluxes at the Geostationary Orbit

The results of cross-correlation analysis between electrons fluxes (with energies of > 0.6MeV, > 2.0 MeV and > 4.0MeV), geomagnetic indices and solar wind parameters are shown in the paper. It is determined that the electron fluxes are controlled not only by the geomagnetic indices, but also by the solar wind parameters, and the solar wind velocity demonstrates the best relation with the electron fluxes. Numerical value of the relation efficiency of external parameters with the highly energetic electrons fluxes shows a periodicity. It is presented here the preliminary results of daily averaged electrons fluxes forecast for a day ahead on the basis of the model of neuron networks.     

加固的多通道多数据类型8毫米磁记录器

鉴于目前压缩预算和削减工程这种情况,遥测和其它数据采集采用低成本记录设备显得极其重要。政府和工业界都希望以小型、便宜的磁记录器取代大型、昂贵的多通道磁记录器。过去许多这类小型磁记录器由于其自身的结构问题,一直局限于记录单通道数据和某一特定的数据类型。 这种8毫米盒式磁记录器过去一直被看作是低成本记录设备,然而采用这种技术的产品在通道数量和数据类型方面受到了严格限制。为解决这一问题,美国马里兰州列克星敦帕克的维达(Veds)公司研制出了一种新的数据采集磁记录器,它采用飞行质量的小型加固机箱封装8毫米磁带机和模块化、可互换的数据输入通道。这些微处理器控制的输入通道能够接收PCM遥测数据、MIL-STD-1553、话音、IRIG时间和ARINC 429/629数据。这种新的结构可将多通道合并到单通道磁带介质上,并可由磁记录器直接重放某些数据类型。本文将讨论这种磁记录器的结构以及在研制中解决的设计问题。     

Detectability of planetary characteristics in disk-averaged spectra. I: The Earth model

Over the next 2 decades, NASA and ESA are planning a series of space-based observatories to detect and characterize extrasolar planets. This first generation of observatories will not be able to spatially resolve the terrestrial planets detected. Instead, these planets will be characterized by disk-averaged spectroscopy. To assess the detectability of planetary characteristics in disk-averaged spectra, we have developed a spatially and spectrally resolved model of the Earth. This model uses atmospheric and surface properties from existing observations and modeling studies as input, and generates spatially resolved high-resolution synthetic spectra using the Spectral Mapping Atmospheric Radiative Transfer model. Synthetic spectra were generated for a variety of conditions, including cloud coverage, illumination fraction, and viewing angle geometry, over a wavelength range extending from the ultraviolet to the farinfrared. Here we describe the model and validate it against disk-averaged visible to infrared observations of the Earth taken by the Mars Global Surveyor Thermal Emission Spectrometer, the ESA Mars Express Omega instrument, and ground-based observations of earthshine reflected from the unilluminated portion of the Moon. The comparison between the data and model indicates that several atmospheric species can be identified in disk-averaged Earth spectra, and potentially detected depending on the wavelength range and resolving power of the instrument. At visible wavelengths (0.4-0.9 microm) O3, H2O, O2, and oxygen dimer [(O2)2] are clearly apparent. In the mid-infrared (5-20 microm) CO2, O3, and H2O are present. CH4, N2O, CO2, O3, and H2O are visible in the near-infrared (1-5 microm). A comprehensive three-dimensional model of the Earth is needed to produce a good fit with the observations.     

Detectability of planetary characteristics in disk-averaged spectra II: synthetic spectra and light-curves of earth

Spatially and spectrally resolved models were used to explore the observational sensitivity to changes in atmospheric and surface properties and the detectability of surface biosignatures in the globally averaged spectra and light-curves of the Earth. Compared with previous efforts to characterize the Earth using disk-averaged models, a more comprehensive and realistic treatment of the surface and atmosphere was taken into account here. Our results are presented as a function of viewing geometry and phases at both visible/near-infrared (0.5-1.7 microm) and mid-infrared (5-25 microm) wavelength ranges, applicable to the proposed NASA-Terrestrial Planet Finder visible coronagraph and mid-infrared interferometer and to the ESADarwin mission architectures. Clouds can change the thermal emission by as much as 50% compared with the cloud-free case and increase the visible albedo by up to 500% for completely overcast cases at the dichotomy phase. Depending on the observed phase and their distribution and type, clouds can also significantly alter the spectral shape. Moreover, clouds impact the detectability of surface biosignatures in the visible wavelength range. Modeling the disk-averaged sensitivity to the "red-edge," a distinctive spectral signature of vegetation, showed that Earth's land vegetation could be seen in disk-averaged spectra, even with cloud cover, when the signal was averaged over the daily time scale. We found that vegetation is more readily discriminated from clouds at dichotomy (50% illumination) rather than at full phase. The detectability of phytoplankton was also explored, but was found to be more difficult to detect in the disk-average than land vegetation.     

2001年航天工艺信息网征文通知

根据2001年3月9日航天工艺信息网网长、在京副网长、联络员工作会议精神，拟定于2001年下半年召开2001年航天工艺学术交流会(具体时间、地点另行通知)。交流会将以崭新的面貌供航天科技人员交流经验、切磋技艺，无疑会对促进和提高航天工艺技术、活跃学术气氛起到积极作用。希望各网员单位和广大科技人员积极投稿，踊跃参加。有关事项通知如下。一、征文内容1．综述航天工艺技术的成就、问题、前景等。2．航天新工艺、新技术、新材料的国外应用情况及其展望。3．精密铸造、焊接、热处理、化铣、超塑成型等特种工艺技术的应用与发展。4．复合…     

A Review of Density Holes Upstream of Earth's Bow Shock

Larmor size transient structures with density depletions as large as 99% of ambient solar wind density levels occur commonly upstream of Earth＇s collisionless bow shock. These ＂density holes＂ have a me...     

对高雷诺数风洞模型表面外形特性测定方法的评定

由于国家跨音速试验设备(简称 NTF,以下同)的高雷诺数,及其伴随薄的边界层,因此,美国国家航空和宇宙航行局正在重新探讨与模型表面形状定义有关的空气动力效应。但目前还没有通过实验证明模型制造车间采用的触针式仪器能准确确定 NTF 模型表面形状的数据。本文叙述了由国家航空和宇宙航行局赞助的,国家标准局正在进行的一项工作。即:评价测量模型表面形状用的触针仪器的性能,和研制出一种新颖的光散射测量仪,它能准确测量表面微观几何形状特性,并克服了触针轮廓仪带来的一些问题。     

雷达系统中最少阵元的天线阵对多重干扰的抑制

1 前言 自适应天线阵因其能有效抑制由主天线方向图旁瓣所接收的强干扰信号，已被广泛用于许多先进的雷达、声纳和通讯系统。在抑制干扰的自适应天线系统中，通常设定阵列是由均匀间隔的阵元组成，并要避免天线方向图中的混淆或栅瓣；设定阵元之间的间隔为波长的一半（λ／2）。其阵元假设相同且为全向的这一阵列结构，称作均匀规整阵列（URA）。然而完全自适应URA的成本和复杂性对于要求大量阵元的某些应用来说是不可能的。