浅析空客飞机污水管路积垢的清洁与预防

对空客飞机污水排污管路内壁积垢的产生原因进行了分析,提出了相应的预防和清洁方法,运用于实际的维护工作中,有利于防止污水管路堵塞,为客舱优质服务提供保障基础。     

一种复杂形体消隐的新方法

本文首先提出了一种视线交点法消隐原理。然后针对复杂形体投影特点,给出了一种消除复杂形体隐藏线的新方法。该方法的特点是将复杂形体分解成若干个若干凸体,并将凸体的外围线框找出,同时将待消隐线段与外围线框求交,并用交点将待消隐线段分解成若干段,每一段采用视线交点法消隐原理测试其可见性,从而达到对待消隐线段消隐的目的。     

航空工业推行清洁生产优先生产线及清洁技术

本文在分析航空工业现状、特点,主要污染源及主要污染物的基础上,对现有清洁技术进行了选择性研究,提出了推行清洁生产的优先生产线及清洁技术。     

飞机中机身壁板预定位柔性工装技术研究

经过对数字化柔性装配工装技术内涵及柔性工装定位方式深入研究,结合某型飞机中机身壁板装配需求,设计了一套壁板组件预定位柔性工装,开发了基于现场总线的多轴控制系统,通过仿真完善了工装设计。工装能与现有自动钻铆机相配合,形成数字化柔性预定位、钻铆生产线,为提高中机身装配质量及效率,缩短生产准备周期,构建飞机数字化柔性装配生产线提供了一个良好范例。     

Probing broad absorption line quasar outflows: X-ray insights

Energetic outflows appear to occur in conjunction with active mass accretion onto supermassive black holes. These outflows are most readily observed in the 10% of quasars with broad absorption lines, where the observer’s line of sight passes through the wind. Until fairly recently, the paucity of X-ray data from these objects was notable, but now sensitive hard-band missions such as Chandra and XMM-Newton are routinely detecting broad absorption line quasars. The X-ray regime offers qualitatively new information for the understanding of these objects, and these new results must be taken into account in theoretical modeling of quasar winds.     

软件插补处理的新方法——比较积分法

本文以直线三坐标，曲线两坐标为例。介绍了一种新型插补方法—比较积分法，用这种插补方法，提高了插补的效率，提高了运动平稳性，使速度均匀。直线插补适合于多坐标联动运动。     

AFM诱导氧化加工Si纳米氧化线的一致性和连续性的研究

研究了在不同的偏置电压和扫描速度下加工的Si氧化线的一致性和均匀性,得到了加工高质量的Si氧化线的实验条件为:偏置电压8V,扫描速度1 μm/s。     

有限元方法设计赋形波束缝隙面阵馈电网络

采用缝隙倾角变化实现幅度加权,采用等高但不等宽的波导实现相位加权,并设计了过渡段以减少反射,可以对赋形波束方向图面阵实现所需要的馈电.为了获得需要的幅度和相位,用有限元方法对缝隙单元尺寸、幅度激励和移相网络进行了数值仿真.通过调整几何尺寸来实现所需要的幅度与相位要求及阻抗匹配.最后给出了1个缝隙阵列天线的设计实例,发现理论计算的赋形方向图与实际测试结果在赋形波束主瓣内吻合很好.     

Measurements of the 12C/13C Ratio in Planetary Nebulae and Implications for Stellar Evolution

We present the results of a study aimed at determining the 12C/13C ratio in two samples of planetary nebulae (PNe) by means of mm-wave observations of 12CO and 13CO. The first group includes six PNe which have been observed in the 3He+ hyperfine transition; the other group consists of 23 nebulae with rich molecular envelopes. We have determined the isotopic ratio in 14 objects and the results indicate a range of values between 9 and 23. In particular, three PNe have ratios well below the value predicted by standard evolutionary models ( 20), indicating that some extra-mixing process has occurred in these stars. We briefly discuss the implications of our results for standard and nonstandard stellar nucleosynthesis.     

The optical emission lines of type 1 X-ray bright Active Galactic Nuclei

A strong X-ray emission is one of the defining signatures of nuclear activity in galaxies. According to the Unified Model for Active Galactic Nuclei (AGN), both the X-ray radiation and the prominent broad emission lines, characterizing the optical and UV spectra of Type 1 AGNs, are originated in the innermost regions of the sources, close to the Super Massive Black Holes (SMBH), which power the central engine. Since the emission is concentrated in a very compact region (with typical size r?0.1$r?0.1$ pc) and it is not possible to obtain resolved images of the source, spectroscopic studies of this radiation represent the only valuable key to constrain the physical properties of matter and its structure in the center of active galaxies. Based on previous studies on the physics of the Broad Line Region (BLR) and on the X-ray spectra of broad (FWHM_Hβ ? 2000 km s⁻¹) and narrow line (1000 km s⁻¹ ?FWHM_Hβ ? 2000 km s⁻¹) emitting objects, it has been observed that the kinematic and ionization properties of matter close to the SMBHs are related together, and, in particular, that ionization is higher in narrow line sources. Here we report on the study of the optical and X-ray spectra of a sample of Type 1 AGNs, selected from the Sloan Digital Sky Survey (SDSS) database, within an upper redshift limit of z=0.35$z=0.35$, and detected at X-ray energies. We present analysis of the broad emission line fluxes and profiles, as well as the properties of the X-ray continuum and Fe Kα emission and we use these parameters to assess the consistency of our current AGN understanding.