BaO-Al_2O_3-SiO_2系玻璃的溶胶-凝胶工艺研究

讨论了多元醇盐水解缩聚的溶胶 -凝胶工艺制备 BAS( Ba O- Al2 O3- Si O2 )玻璃时 ,加水方式和加水量 ,醇盐含量和醇盐酸碱性、溶剂含量以及陈化温度对凝胶形成、胶凝时间和凝胶玻璃结构的影响。实验成分范围 ( wt% )为 Si O2 ∶ 34～ 5 0 ,Al2 O3∶ 1 0～ 30 ,Ba O∶ 2 4～ 48,Li2 O∶ 0～ 5。结果表明 ,采用正硅酸乙酯预水解方式 ,水和醇盐摩尔比 >6～ 8,正硅酸乙酯 >40 mol%或异丙醇铝 <40 mol% ,可以获得具有 80 %以上架状、纯架状网络结构 ,断键程度 <1 2 %的均匀透明凝胶玻璃。增加加水量和提高陈化温度可以缩短胶凝时间     

浅析民用运输类飞机机体防冰的适航新规章

2009年8月3日,美国联邦航空局（FAA）在联邦注册报上发布了联邦航空条例FAR25部第25-129号修正案—＂结冰保护的启动＂,对运输类飞机结冰探测方式和结冰保护系统（IPS）工作方式提出了明确要求。阐述了第25-129号修正案颁布前机体防冰及相关规章的演变历史,在对该修正案研究的基础上,提出了新规章推出后对防冰系统适航要求的关键点,以及机体防冰相关规章的发展趋势,供系统设计和适航审查参考。     

智能交通系统(ITS)的发展 及其模型化研究

智能交通系统在欧洲也称道路交通信息通讯系统,是基于系统工程、电子、通信、信息等多种高新技术,并已渗透到航空、水运、铁路交通领域的新型交通系统.ITS的建立可以提高路网通行能力和服务水平,改善环保质量,提高能源利用率.介绍其基本概念以及国内外发展的概况后,提出了智能交通系统的学科体系模型、服务功能模型和网络层次模型,并简要分析了模型化的意义.最后,对系统的标准化问题及模型化研究对标准化的作用作了简单地介绍.     

冷贮备可修系统的维修更换模型

研究了由一个修理工、两同型部件组成的冷贮备可修系统,在故障部件不能"修复如新"的条件下,分别选择系统中部件1的故障次数N和总工作时间T为更换策略,利用更新过程和几何过程理论,选择最优的策略N*和T*,使得系统经长期运行单位时间内平均停机时间最短,并推导出了系统经长期运行单位时间内平均停机时间的表达式。最后,通过数值例子对所得结果进行了分析。     

Effect of pitch angle on initial stage of a transport airplane ditching

Airworthiness regulations require that the transport airplane should be proved to ensure the survivability of the ditching for the passengers. The planned ditching of a transport airplane on the calm water is numerically simulated. The effect of pitch angle on the impact characteristics is especially investigated by a subscaled model. The Reynolds-averaged Navier-Stokes (RANS) equations of unsteady compressible flow are solved and the realizable j-e equations are employed to model the turbulence. The transformation of the air-water interface is tracked by volume of fluid (VOF) model. The motion of the rigid body is modeled by dynamic mesh method. The initial ditching stage of the transport airplane is analyzed in detail. The numerical results show that as the pitching angle increases, the maximal normal force decreases and the pitching motion becomes much gentler. The aft fuselage would be sucked down by the water and lead to pitching up, whereas the low horizontal tail prevents this trend. Consequently, the transport aircraft with low horizontal tail should ditch on the water at an angle between 10 and 12 as a recommendation.     

The STARK-B database as a resource for “STARK” widths and shifts data: State of advancement and program of development

“Stark” broadening theories and calculations have been extensively developed for about 50 years and can now be applied to many needs, especially for accurate spectroscopic diagnostics and modeling. This requires the knowledge of numerous collisional line profiles. Nowadays, the access to such data via an online database becomes essential. STARK-B is a collaborative project between the Astronomical Observatory of Belgrade and the Laboratoire d’Étude du Rayonnement et de la matière en Astrophysique (LERMA). It is a database of calculated widths and shifts of isolated lines of atoms and ions due to electron and ion collisions (impacts). It is devoted to modeling and spectroscopic diagnostics of stellar atmospheres and envelopes, laboratory plasmas, laser equipments and technological plasmas. Hence, the domain of temperatures and densities covered by the tables is wide and depends on the ionization degree of the considered ion. STARK-B has been fully opened since September 2008 and is in free access.     

Statistical validation of HZETRN as a function of vertical cutoff rigidity using ISS measurements

Measurements taken in Low Earth Orbit (LEO) onboard the International Space Station (ISS) and transit vehicles have been extensively used to validate radiation transport models. Primarily, such comparisons were done by integrating measured data over mission or trajectory segments so that individual comparisons to model results could be made. This approach has yielded considerable information but is limited in its ability to rigorously quantify and differentiate specific model errors or uncertainties. Further, as exploration moves beyond LEO and measured data become sparse, the uncertainty estimates derived from these validation cases will no longer be applicable. Recent improvements in the underlying numerical methods used in HZETRN have resulted in significant decreases in code run time. Therefore, the large number of comparisons required to express error as a function of a physical quantity, like cutoff rigidity, are now possible. Validation can be looked at in detail over any portion of a flight trajectory (e.g. minute by minute) such that a statistically significant number of comparisons can be made. This more rigorous approach to code validation will allow the errors caused by uncertainties in the geometry models, environmental models, and nuclear physics models to be differentiated and quantified. It will also give much better guidance for future model development. More importantly, it will allow a quantitative means of extrapolating uncertainties in LEO to free space. In this work, measured data taken onboard the ISS during solar maximum are compared to results obtained with the particle transport code HZETRN. Comparisons are made at a large number (∼77,000) of discrete time intervals, allowing error estimates to be given as a function of cutoff rigidity. It is shown that HZETRN systematically underestimates exposure quantities at high cutoff rigidity. The errors are likely associated with increased angular variation in the geomagnetic field near the equator, the lack of pion production in HZETRN, and errors in high energy nuclear physics models, and will be the focus of future work.     

Comparison of the transport codes HZETRN,HETC and FLUKA for galactic cosmic rays

The HZETRN deterministic radiation code is one of several tools developed to analyze the effects of harmful galactic cosmic rays (GCR) and solar particle events on mission planning and shielding for astronauts and instrumentation. This paper is a comparison study involving the two Monte Carlo transport codes, HETC–HEDS and FLUKA and the deterministic transport code, HZETRN. Each code is used to transport an ion from the 1977 solar minimum GCR spectrum impinging upon a 20 g/cm² aluminum slab followed by a 30 g/cm² water slab. This research is part of a systematic effort of verification and validation to quantify the accuracy of HZETRN and determine areas where it can be improved. Comparisons of dose and dose equivalent values at various depths in the water slab are presented in this report. This is followed by a comparison of the proton and forward, backward and total neutron flux at various depths in the water slab. Comparisons of the secondary light ion ²H, ³H, ³He and ⁴He fluxes are also examined.     

Observations of the Sun at Vacuum-Ultraviolet Wavelengths from Space. Part II: Results and Interpretations

In Part I of this review, the concepts of solar vacuum-ultraviolet (VUV) observations were outlined together with a discussion of the space instrumentation used for the investigations. A section on spectroradiometry provided some quantitative results on the solar VUV radiation without considering any details of the solar phenomena leading to the radiation. Here, in Part II, we present solar VUV observations over the last decades and their interpretations in terms of the plasma processes and the parameters of the solar atmosphere, with emphasis on the spatial and thermal structures of the chromosphere, transition region and corona of the quiet Sun. In addition, observations of active regions, solar flares and prominences are included as well as of small-scale events. Special sections are devoted to the elemental composition of the solar atmosphere and theoretical considerations on the heating of the corona and the generation of the solar wind.     

Element Settling in the Solar Interior

Element settling inside the Sun now becomes detectable from the comparison of the observed oscillation modes with the results of the theoretical models. This settling is due, not only to gravitation, but also to thermal diffusion and radiative acceleration (although this last effect is small compared to the two others). It leads to abundance variations of helium and heavy elements of ≅ 10% below the convective zone. Although not observable from spectroscopy, such variations lead to non-negligible modifications of the solar internal structure and evolution. Helioseismology is a powerful tool to detect such effects, and its positive results represent a great success for the theory of stellar evolution. Meanwhile, evidences are obtained that the element settling is slightly smoothed down, probably due to mild macroscopic motions below the convective zone. Additional observations of the abundances of both 7Li and 3He lead to specific constraints on these particular motions. This revised version was published online in June 2006 with corrections to the Cover Date.