Ozone mini-hole observation over the Balkan Peninsula in March 2005

Areas with dimensions of 1000–3000 km in which the total ozone content (TOC) decreases fast are called ozone mini-holes. They are generated mainly dynamically in two ways, either by poor-ozone air mass transport from the tropics to higher latitudes by planetary wave activity or, they are connected with strong adiabatic uplifting of the tropopause height. An ozone mini-hole, generated by the second mechanism, was observed over the Balkan Peninsula on 19/21 March 2005. In the middle of March, the polar vortex was strongly disturbed by Rossby waves, reaching up to the lower stratosphere. Warming episodes over a geographical area, covering the Barents Sea and the Polar Sea north from Central Siberia, displaced a polar vortex fragment extremely southwards. However, the vorticity was weak and the stratospheric temperatures did not reach low values, providing conditions for ozone chemical destruction via heterogenic reactions. At the same time, a Rossby wave ridge was located below the European polar fragment. In the period from 13 to 19 March, the thermal tropopause over Sofia was uplifted almost by 3 km. Ozone distributions observed by the SCIAMACHY instrument on 18–21 March show a fast TOC decrease westwards from Ireland, which was moving eastwards during the next days, increasing the area in which the ozone content decreased. On 20/21 March low ozone content was observed above the Stara Zagora (42°N, 25°E) ground-based station by means of the GASCOD instrument, using DOAS technique. The TOMS Earth probe instrument detected 237 DU over Sofia. This is a record low March value from the beginning of the TOMS instrument measurements in 1978. In March/April the ozone distribution was characterized by its mean annual maximum of 360 DU at 42°N.     

UVCS/SOHO Observations of H I Lyman Alpha Line Profiles in Coronal Holes at Heliocentric Heights Above 3.0 R⊙

The Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO) has been used to measure spectral line profiles for H I Lyα in the south polar coronal hole at projected heliocentric heights from 3.5 to 6.0 R_⊙ during 1998 January 5–11. Observations from 1.5 to 2.5 R_⊙ were made for comparison. The H I Lyα profile is the only one observable with UVCS above 3.5 R_⊙ in coronal holes. Within this region the outflowing coronal plasma becomes nearly collisionless and the ionization balance is believed to become frozen. In this paper, the 1/e half widths of the coronal velocity distributions are provided for the observed heights. The velocity distributions include all motions contributing to the velocities along the line of sight (LOS). The observations have been corrected for instrumental effects and interplanetary H I Lyα. The half widths were found to increase with projected heliographic height from 1.5 to 2.5 R_⊙ and decrease with height from 3.5 to 5 R_⊙. This revised version was published online in June 2006 with corrections to the Cover Date.     

O-star winds in the Magellanic Clouds and the Milky Way

UV P-Cygni profiles of OB-stars in the Magellanic Clouds (observed with HST), and the galaxy (observed with IUE) are analyzed empirically using a line formation procedure similar to the one described by Lamers et al. (1987). The assumption of a constant microturbulencev _turb throughout the wind is dropped and replaced by a radially increasing turbulence parameterv _turb(v), thus improving the fit for the emission peaks substantially, and at the same time avoiding the need for a justification of extremely supersonic turbulence in the vicinity of the wind's sonic point. The Sobolev optical depth is determined interatively at fixed velocities in the wind, which removes the bias introduced by the choice of a specific parameterization function. Where it was possible and necessary a full photospheric spectrum was used to illuminate the wind line. The terminal velocitiesv are are found to be largest in the Galaxy, smallest in the Small Magellanic Cloud, and intermediate or similar to galactic in the Large Cloud.     

UV光固化胶粘剂的研制

研制出了一种适用于高档家具玻璃、玻璃工艺器、水晶玻璃，光学玻璃等胶接用的丙烯酸系UV光固化胶粘剂，该胶粘接强度高、耐水性能好，玻璃接头在沸水中煮数十小时不剥离。     

基于电化学沉积的高深宽比无源MEMS惯性开关的研制

基于电化学沉积技术在金属基底上制作了一种新型的无源MEMS惯性开关。针对高深宽比、细线宽微电铸用光刻胶模具制作过程中,由于SU-8胶膜严重侧蚀导致的胶膜制作困难、质量低下的问题,进行了紫外光刻试验研究。试验研究了不同曝光剂量和后烘时间对SU-8胶光刻效果的影响,优化了光刻工艺参数。采用降低曝光剂量和延长后烘时间相结合的方法解决了高深宽比、细线宽SU-8胶膜制作困难的问题,制作出高质量的微电铸用光刻胶模具。最后,在上述试验结果基础上制作了一种高深宽比、无源MEMS惯性开关。其外形尺寸为3935μm×3935μm×234μm,其中最细线宽12μm,单层最大深宽比达10∶1,多层最大深宽比达20∶1。     

基于proteus的51单片机16×64LED的设计

介绍基于51单片机的16×64LED点阵显示屏的设计,在这里给出其原理图以及程序流程图。在Proteus7.5软件当中进行原理图的绘制,利用汉字转换软件将汉字转换为将要发送给单片机的点阵数据,在keil软件当中采用C语言编程,与proteus进行联调,并通过仿真软件Proteus7.5,最终实现自己设想的效果,总体上系统的设计简单、显示清晰、成本较低。     

民用飞机驾驶舱照明光辐射安全问题探讨The Discussion of Civil Aircraft Cockpit Lighting light radiation safety issue 魏培坤 吴春泽

民用飞机驾驶舱照明旨在为飞行员创造一个舒适安全的视觉环境,保证飞行员能准确地操作各种控制开关和清晰地判读仪表、显示器等的显示信息。照明的安全除了传统意义上的安全外也应包括光辐射安全,随着LED在驾驶舱照明中的应用,光辐射安全问题日益突出,必须制定出一种对驾驶舱照明环境中的光辐射危害水平进行评估的方法,以保证飞行员的眼睛和皮肤不受到潜在的光辐射伤害。     

MSM结构ZnO紫外探测器的制备及光电性能研究

采用磁控溅射方法,在石英衬底上制备了光电性能优良的ZnO紫外探测器。通过紫外光电性能测试、扫描电子显微镜(SEM)观察及X射线衍射(XRD)分析,研究了ZnO紫外探测器的光电特性。结果表明:探测器的光电流高出暗电流近3个数量级,紫外波段的光响应高出可见光波段近2个数量级,所制备ZnO紫外探测器达到了高辐射灵敏度和可见盲特性的要求。     

R3D-B2 – Measurement of ionizing and solar radiation in open space in the BIOPAN 5 facility outside the FOTON M2 satellite

Solar and space radiation have been monitored using the R3D-B2 radiation risks radiometer-dosimeter on board a recent space flight on the Russian satellite Foton M2 within the ESA Biopan 5 facility mounted on the outside of the satellite exposed to space conditions. The solar radiation has been assayed in four wavelength bands (UV-C, 170–280 nm, UV-B, 280–315 nm), UV-A (315–400 nm) and PAR (photosynthetic active radiation, 400–700 nm). The data show an increasing tumbling rotation of the satellite during the mission. The photodiodes do not show a cosine response to the incident light which has been corrected. After calibration of the signals using the extraterrestrial spectrum, doses have been calculated for each orbit, for each day and for the total mission as basic data for the biological material which has been exposed in parallel in the Biopan facility. Cosmic ionizing radiation has been monitored and separated in 256 deposited energy spectra, which were further used for determination of the absorbed dose rate and flux. Basic data tables were prepared to be used by other Biopan 5 experiments. The paper summarizes the results for the Earth radiation environment at the altitude (262–304 km) of the Foton M2 spacecraft. Comparisons with the predictions of NASA Earth radiation environment experimental models AE-8 and AP-8, and the PSB97 model are also presented, which calculate the fluxes of ionizing radiation from a simulation. AP-8 is a model for trapped radiation.