The Swift Ultra-Violet/Optical Telescope

The Ultra-Violet/Optical Telescope (UVOT) is one of three instruments flying aboard the Swift Gamma-ray Observatory. It is designed to capture the early (∼1 min) UV and optical photons from the afterglow of gamma-ray bursts in the 170–600 nm band as well as long term observations of these afterglows. This is accomplished through the use of UV and optical broadband filters and grisms. The UVOT has a modified Ritchey–Chrétien design with micro-channel plate intensified charged-coupled device detectors that record the arrival time of individual photons and provide sub-arcsecond positioning of sources. We discuss some of the science to be pursued by the UVOT and the overall design of the instrument.     

基于Pro/E软件的电解加工夹具的参数化设计

应用Pro/E软件进行复杂型腔电解加工夹具的设计，通过夹具零件的造型、组装及组件的静态、动态分析，阐述了在Pro/E软件平台上进行夹具设计的主要过程、特点及优越性。它不同于以往机械设计二维CAD软件，避免了因漏掉相关零件的修改而在零件实际装配时所带来的干涉现象。保证了设计结果的准确性，并提高了设计效率。在电解加工复杂整体构件组合电加工数字化制造中得到应用，并取得很好的效果。     

航空静止变流器电路的系统设计方案研究

研究了静止变流器电路的系统设计问题,对航空静止变流器的SPWM直接升压设计方案和间接升压设计方案进行了比较研究,研究的重点是电路的变换效率。根据电路特性,进行了理论分析,指出了两者的基本区别在于阻抗匹配和波形变换。通过实验研究和理论分析发现,SPWM直接升压电路系统虽然系统设计简单,但是变换效率较低;间接升压系统电路的设计比较复杂,变换效率较高,而且中间高压直流环节不能省略。     

海洋环境下机载电连接器腐蚀分析与失效机理

为分析海洋环境对机载航空电连接器的腐蚀情况的影响,将电连接器进行自然暴晒试验和实验室多应力加速试验,采用扫描电子显微镜(SEM)、X射线能谱仪(EDS)和光学显微镜等表征手段对试验件腐蚀程度、腐蚀区的微量元素定性定量分析。结果显示,电连接器的中间轴身和头部高应力接触区易发生腐蚀。电连接器主要的腐蚀方式有电应力腐蚀和电化学腐蚀。高温、高盐、高湿和高辐射的海洋环境加速了电连接器被腐蚀的过程。被腐蚀的电连接器局部镀层破损甚至脱落,基底材料暴露在外且被腐蚀和破坏,并形成大量的金属盐腐蚀产物,导致失效概率增加。出现失效的主要原因是电连接器的接触电阻增加、绝缘性能降低、电偶腐蚀、应力松弛和蠕变。     

活笥银粉中微量铜铁的测定

提出用空气－乙炔火焰原子吸收光谱法来测定银锌电池活性银粉中的微量铜铁，并对测定条件和干扰因素进行了综合考虑，该测定方法具有灵敏度、精确度高，干扰小，选择性和重现性好等优点。测定样品微量铜铁含量的相对标准偏差均小于１.5%(n=8）。标准加入回收率均在（９７.00-102.00)%(n=5)范围内，完全适用于银锌电池活性银粉中微量铜铁含量的控制和样品系统分析，实际应用中取得了很好的效果。     

结构吸波材料多层阻抗渐变设计及应用

对多层阻抗渐变的吸波结构设计思想进行了分析,介绍了多层阻抗渐变思想在吸波层板和泡沫两类结构吸波材料设计上的应用。理论计算与试验验证结果均表明,采用多层阻抗渐变设计能够使吸波层板和泡沫的吸波带宽向低频拓展,同时显著提高吸波泡沫的吸收强度。具有三个阻抗渐变吸收层的4 mm厚吸波层板在5~18 GHz频段反射率小于-10 d B;具有六个阻抗渐变吸收层的22 mm厚吸波泡沫在2~18 GHz频段反射率小于-10 d B,其中在6~18 GHz频段反射率小于-20 d B,8~12 GHz频段反射率小于-30 d B。多层阻抗渐变设计是提高结构吸波材料吸波性能的有效手段。     

XANES analysis of organic residues produced from the UV irradiation of astrophysical ice analogs

Organic residues formed in the laboratory from the ultraviolet (UV) photo-irradiation or ion bombardment of astrophysical ice analogs have been extensively studied for the last 15 years with a broad suite of techniques, including infrared (IR) and UV spectroscopies, as well as mass spectrometry. Analyses of these materials show that they consist of complex mixtures of organic compounds stable at room temperature, mostly soluble, that have not been fully characterized. However, the hydrolysis products of these residues have been partly identified using chromatography techniques, which indicate that they contain molecular precursors of prebiotic interest such as amino acids, nitrile-bearing compounds, and amphiphilic compounds. In this study, we present the first X-ray absorption near-edge structure (XANES) spectroscopy measurements of three organic residues made from the UV irradiation of ices having different starting compositions. XANES spectra confirm the presence of different chemical functions in these residues, and indicate that they are rich in nitrogen- and oxygen-bearing species. These data can be compared with XANES measurements of extraterrestrial materials. Finally, this study also shows how soft X rays can alter the chemical composition of samples.     

Constraints on Coronal Outflow Velocities Derived from UVCS Doppler Dimming Measurements and in-Situ Charge State Data

We constrain coronal outflow velocity solutions, resolved along the line-of-sight, by using Doppler dimming models of H I Lyman alpha and O VI 1032/1037 Å emissivities obtained with data from the Ultraviolet Coronagraph Spectrometer (UVCS) on SOHO. The local emissivities, from heliocentric heights of 1.5 to 3.0 solar radii, were determined from 3-D reconstructions of line-of-sight intensities obtained during the first Whole Sun Month Campaign (10 August to 8 September 1996). The models use electron densities derived from polarized brightness measurements made with the visible light coronagraphs on UVCS and LASCO, supplemented with data from Mark III at NCAR/MLSO. Electron temperature profiles are derived from 'freezing-in' temperatures obtained from an analysis of charge state data from SWICS/Ulysses. The work concentrates on neutral hydrogen outflow velocities which depend on modeling the absolute coronal H I Lyα emissivities. We use an iterative method to determine the neutral hydrogen outflow velocity with consistent values for the electron temperatures derived from a freezing-in model.     

The Solar Wind and the Sun in the Past

Exposure to the solar wind can have significant long term consequences for planetary atmospheres, especially for planets such as Mars that are not protected by global magnetospheres. Estimating the effects of solar wind exposure requires knowledge of the history of the solar wind. Much of what we know about the Sun’s past behavior is based on inferences from observations of young solar-like stars. Stellar analogs of the weak solar wind cannot be detected directly, but the interaction regions between these winds and the interstellar medium have been detected and used to estimate wind properties. I here review these observations, with emphasis on what they suggest about the history of the solar wind.