涡轮盘低循环疲劳可靠性设计方法

基于现有疲劳试验数据,建立了涡轮盘材料GH4133合金的循环应力-应变概率模型,并提出涡轮盘低循环疲劳可靠性设计方法。以有限元分析软件ANSYS为平台,利用APDL语言进行了涡轮盘3维参数化建模;通过灵敏度分析确定了涡轮盘结构概率分析中的主要影响参数;通过涡轮盘结构低循环疲劳可靠性分析和关键结构几何参数的反复修改,满足了涡轮盘的疲劳可靠性设计指标。该方法可为发动机其他关键结构的疲劳可靠性设计分析提供参考。     

模拟飞机迎风面三维积冰的数学模型

针对飞机迎风面的积冰建立了三维积冰模型,给出了模型的求解方法和求解步骤.该模型不但可以模拟明冰积冰、霜冰积冰和不结冰三种情况下的冰层生长,还可以模拟未凝结水膜在冰层表面的流动,而且在求解过程中可以自动判断过冷水滴撞击到迎风面以后的积冰形态.利用该模型数值模拟了翼型与平板相正交而形成的简单三维结构上的积冰过程,并将所得结果中翼型上三维冰形的二维截面与美国航空航天局(NASA)的冰形进行了对比,获得了较好的一致性,证实了所建立的积冰模型是合理的.      

叶-盘系统振动特性有限元分析程序实现

引入空间八节点等参数单元,对叶-盘结构进行了有限元网格划分.利用自行编制的有限元循环对称结构振动分析程序对叶-盘结构(泵叶轮及涡轮叶轮)进行了振动特性分析,并与ANSYS软件计算结果进行了对比.经过对比,本程序的计算结果与ANSYS软件的计算结果吻合良好,从而验证了本计算程序具有良好的工程计算精度.     

应用基于FEM的预成形最优化方法提高锻件变形均匀性

锻件变形分布不均匀将导致锻件各部位的组织和性能产生很大差异。应用基于正向有限元数值模拟和最优化方法进行坯料预成形设计的新方法,可显著提高锻件各部位的变形均匀性。首先介绍了以提高锻件变形分布均匀性为目的的坯料预成形最优化方法的基本原理,并针对典型的IN718合金涡轮盘锻件进行了坯料预成形设计。给出了预成形坯料与普通圆柱坯料的对比结果,并进行了相应的试验验证。结果表明,应用这种方法对IN718合金涡轮盘锻件进行坯料预成形设计,可使盘锻件各部位变形均匀性明显改善。     

某型燃气轮机封严盘疲劳裂纹机理分析

为了系统研究某型燃气轮机封严盘疲劳故障的现象、机理、特点和原因,进行了封严盘故障损伤痕迹、断口形貌、材料成分、金相组织等分析;同时进行了强度(应力)和模态振动特性方面的有限元计算研究,在此基础上进行了共振特性分析。分析结果表明:该封严盘结构设计存在薄弱环节,其均压孔孔边径向应力水平高,孔边表面状态不佳,在一定振动应力作用下,均压孔边容易产生高周性质的疲劳裂纹。对防止某型燃气轮机封严盘产生疲劳裂纹失效提出修理和使用中应控制的要点。     

Black-hole transients: From QPOs to relativistic jets

Due to the impressive amount of new data provided by the RXTE satellite in the past decade, our knowledge of the phenomenology of accretion onto black holes has increased considerably. In particular, it has been possible to schematize the outburst evolution of transient systems on the basis of their spectral and timing properties, and link them to the ejection of relativistic jets as observed in the radio. Here, I present this scheme, concentrating on the properties of the quasi-periodic oscillations observed in the light curves and on the link with jet ejection.     

Fluid instabilities around accreting X-ray sources

Some aspects of fluid instabilities occurring in the magnetospheres of accreting neutron stars are discussed. It is pointed out that (i) in the absence of strong differential rotation, the accreting plasma should be drawn out into spiralling, sheet-like structures, resulting in efficient mixing between the two media; (ii) the Rayleigh-Taylor instability also acts to limit the X-ray luminosity in super-critical sources; and (iii) magnetic shear has a strong stabilizing influence on Kelvin-Helmholtz modes, and its presence may allow substantial amounts of material to be supported around the magnetosphere.     

Energy release in stellar magnetospheres

The interaction of a stellar magnetosphere with a thin accretion disk is considered. Specifically, I consider a model in which (1) the accretion disk is magnetically linked to the star over a large range of radii and (2) the magnetic diffusivity of the disk is sufficiently small that there is little slippage of field lines within the disk on the rotation time scale. In this case the magnetic energy built up as a result of differential rotation between the star and the disk is released in quasi-periodic reconnection events occuring in the magnetosphere (Aly and Kuijpers 1990). The radial transport of magnetic flux in such an accretion disk is considered. It is show that the magnetic flux distribution is stationary on the accretion time scale, provided the time average of the radial component of the field just above the disk vanishes. A simple model of the time-dependent structure of the magnetosphere is presented. It is shown that energy release in the magnetosphere must take place for (differential) rotation angles less than about 3 radians. The magnetic flux distribution in the disk depends on the precise value of the rotation angle.     

两种信道编码记录方式在光盘应用中的对比

依据数字编码理论对几种光盘编码调制的结构参数性能进行了比较，着重分析了光盘的两种信道编码记录方式：用于磁光（ＭａｇｎｅｔｏＯｐｔｉｃａｌｄｉｓｋ－ＭＯ）光盘的游程长度受限（ＲｕｎＬｅｎｇｔｈＬｉｍｉｍｔｅｄ）脉宽调制（ＰｕｌｓｅＷｉｄｔｈＭｏｄｕｌａｔｉｏｎ）［ＲＬＬ（１，７）－ＰＷＭ］记录方式，及用于相变（ＰｈａｓｅＣｈａｎｇｅ－ＰＣ）光盘的游程长度受限（ＲｕｎＬｅｎｇｔｈＬｉｍｉｍｔｅｄ）脉位调制（ＰｕｌｓｅＰｏｓｉｔｉｏｎＭｏｄｕｌａｔｉｏｎ）［ＲＬＬ（２，７）－ＰＰＭ］记录方式，并结合记录介质的特点，阐明了两者并存的原因．     

Black hole accretion and X-ray spectra of QSOS

Changes in Eddington accretion ratios are thought to result in X-ray spectral index changes in Galactic binary black hole systems. Objects with higher Eddington ratios have softer X-ray spectra. Can we apply this result to much more massive black hole systems such as QSOs? If so, X-ray observations will give us valuable insight into the physics of QSOs. Among QSOs, X-ray spectral index is part of a large set of correlated optical and UV observational properties, especially optical Fe II and [O III] strengths in the Hβ region. To investigate whether this set of correlations is related to Eddington ratio, we use as probes, BALQSOs that have been suggested to be youthful super-accretors. We conducted infrared spectroscopy of the Hβ rest wavelength region for a sample of BALQSOs and compared line measurements with those for high and low redshift non-BAL QSOs. Hβ line widths and bolometric luminosity are used to calculate QSO black hole masses and Eddington ratios. Our results support the hypothesis that optical Fe II and [O III] line strengths are Eddington ratio indicators in QSO central engines. A possible explanation is that strong Fe II and weak [O III] indicate abundant cold gas that could fuel near Eddington accretion.