KFTA太阳模拟器灯单元的方案设计

在进行KFTA太阳模拟器的设计中,首次采用了氙灯水平点燃的灯单元设计方案。氙灯水平点燃既可以提高太阳模拟器的能量利用率,又降低了成本,节省了人力、物力,但同样也面临着许多新的问题：灯的选择、灯的稳弧、灯的水平调节机构以及灯的应力分析等。文章正是从以上各个方面阐述了KFTA太阳模拟器灯单元的设计思想及方法。     

卫星动不平衡方法研究

文章结合在工程中遇到的动不平衡实际问题,根据平衡机的基本工作原理,提出了双平面分别配重、合成计算的解决思路,并在理论上对自旋稳定卫星的双平面配重的动不平衡配重的计算方法进行了分析和研究,验证了配平计算方法的正确性和可行性。最后,根据配重计算方法提出了配重调整的工艺步骤。     

航天器总装过程风险分析和工艺安全性设计

文章分析了航天器总装过程中的危险因素以及各总装作业单元的危险程度及危害性,阐述了总装工艺安全性设计的方法和意义,建议构建安全控制要素基础数据库,进行工艺安全分析和安全技术评价,以期为航天器总装的安全性设计提供参考。     

高校英语专业开展通识教育的实践探索

本文着眼于高校外语专业的发展,以通识性教育为切入点,并以北华航天工业学院外语系为研究对象,通过课堂形式,课堂内容,师资建设三方面开展实践研究和探索,分析其成功经验和不足,并对高校外语专业通识化教育发展提出合理化建议,尝试性构建专业教育+通识教育发展的新模式,进一步推动高校外语专业教学改革的步伐。     

Understanding solar streamers: The role of SOHO

Streamers have been observed since far back in time, but our knowledge of their morphology and of their physical characteristics is still very limited. As a consequence, the present streamer picture is largely incomplete: because individual features are poorly known, their role in more general phenomena (like the evolution of the global corona or the solar wind mass and flow pattern) is also poorly known. In this presentation, the more relevant open problems in the understanding of streamers will be illustrated and it will be shown how new data acquired by SOHO may help us to reach a better understanding of these structures.     

XMM-Newton observations across the Cygnus Loop from northeastern rim to southwestern rim

We have observed the Cygnus Loop from the northeast (NE) to the southwest (SW) with XMM-Newton. We extracted spectra from 3′-spaced annular regions across the Loop and fitted them either with a one-kT_e-component non-equilibrium ionization (NEI) model or with two-kT_e-component NEI model. We found that the two-kT_e-component model yields significantly better fits in almost all the spectra than the one-kT_e-component model. Judging from the abundances, the high-kT_e-component in the two-temperature model must be fossil ejecta while the low-kT_e-component comes from the swept-up interstellar medium (ISM). The distributions of Ne, Mg, Si, and S for fossil ejecta appear to retain the onion-skin structure at the time of a supernova explosion, suggesting that significant overturning of the ejecta has not occurred yet. Comparing the relative abundances of fossil ejecta estimated for the entire Cygnus Loop with those from theoretical calculations for Type-II SN, the mass of the progenitor star is likely to be ∼13 M_⊙. The trends of the radial profiles of kT_e and emission integral for the swept-up ISM are adequately described by the Sedov model, suggesting that the swept-up ISM is concentrated in a shell-like structure. Comparing our data with the Sedov model, we found the ambient medium density to be ∼0.7 cm⁻³. Then, we estimated the total mass of the swept-up ISM and the age of the remnant to be ∼130 M_⊙ and 13,000 years, respectively. Note that if the explosion occurred within a stellar wind cavity, then the density in the cavity, the total swept-up mass in the cavity, and the age of the remnant are estimated to be ∼0.14 cm⁻³, ∼25 M_⊙, and ∼10,000 years, respectively.     

浅谈现阶段的普通工科院校学生管理工作存在的问题及对策

受多种因素的影响,现阶段高校学风总体状态呈现下滑趋势。这无疑是给高校学生管理工作者提出了一个＂如何扭转学风下滑现状,不断提高学生管理工作水平＂的新任务。以普通工科院校为对象,在对学风建设和学生管理工作现状进行比较全面的调查分析基础上,提出了五种改善和加强普通工科院校学风建设和学生管理工作的有效途径。     

应用试验模态参数修正理论模型的最佳矩阵逼近法

本文从特征方程和模态正交性条件出发，给出了一种应用模态参数识别结果修正理论模型的最佳矩阵逼近方法。该方法通过对识别出的模态矩阵进行奇异值分解并结合特征方程和模态正交条件导出了修正理论模型的通解表达式，在此基础上，给出了最佳逼近解的定义，研究了最佳逼近解的唯一性，给出了最佳修正质量矩阵和刚度矩阵的具体表达式，数值计算表明，本文方法具有很高的修正精度，对于大误差模型也有较好的修正能力，具有一定的应有和     

Wolf-Rayet stars in starbursts

Let us suppose that it is possible observationally to determine the number ratio of WR to O stars in a starburst galaxy (cf. e. g. Vacca &; Conti 1992) and that one can also have some information on the way the different WR subtypes are distributed (number ratios as WN/WR, WNL/WR etc ...), the question is, what can we deduce from these values on the burst of star formation which gave birth to these WR stars? Is it possible for instance to constrain the age of the burst (i.e. the time elapsed since the beginning of the burst of star formation), its intensity (i.e. the ratio of the star formation rate during the burst to that before the burst) or the metallicity of the cloud from which the stars formed? We present here models of starbursts based on the most recent models for single stars computed by the Geneva group and show that the study of the WR population in a starburst provides very useful insights on the age of the burst and on the metallicity of the star forming zone.     

Hydrodynamic atmosphere models for hot luminous stars II. Method and improvements over unified models

In a paper submitted to A&A we present the first line blanketed hydrodynamic models of spherically expanding atmospheres of hot stars. This paper is complementary to the submitted paper. Here, we emphasize the advantages and the weak points of our approach and we present additional technical aspects.The models are characterised by a simultaneous solution of the equation of motion, the non-LTE populations of H and He, and radiation transfer in a line blanketed atmosphere. The entire domain from the optically thick photosphere out to the terminal velocity of the wind is treated. The radiative forces are evaluated consistently with the depth-dependent radiation field, taking into account multiple scattering by metal lines and line overlap.