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.     

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.     

The case for massive,evolving winds in black hole X-ray binaries

In the last decade, high-resolution X-ray spectroscopy has revolutionized our understanding of the role of accretion disk winds in black hole X-ray binaries. Here I present a brief review of the state of wind studies in black hole X-ray binaries, focusing on recent arguments that disk winds are not only extremely massive, but also highly variable. I show how new and archival observations at high timing and spectral resolution continue to highlight the intricate links between the inner accretion flow, relativistic jets, and accretion disk winds. Finally, I discuss methods to infer the driving mechanisms of observed disk winds and their implications for connections between mass accretion and ejection processes.     

机翼积冰数值模拟

采用计算流体力学（CFD）方法对三段翼和MS-317后掠翼进行了积冰数值模拟研究,基于欧拉两相流理论,应用分区算法,对空气流场和水滴流场进行了数值求解,得到水滴收集率.求解3-D积冰模型得到积冰量.将MS-317的冰形计算结果与实验数据以及软件LEWICE3D的计算结果进行了对比.结果显示:三维积冰模型具有较好的精度,虽然预测的冰形与实验数据有一些差异,最大厚度方面,误差在13.1%以内,但是积冰的类型与体积和实验数据基本一致.      

基于CFD的机翼结冰过程分析

采用一种适用于分析机翼结冰过程的数值模拟方法,该方法在飞机结冰气象条件下采用计算流体力学（Computational Fluid Dynamics,CFD）对机翼流场进行计算,获得流场中二维机翼翼型的水滴撞击特性,并遵循质量和能量守恒方程,计算出机翼表面的结冰量,预测出机翼的积冰形状。所得冰形与文献中的试验数据吻合良好,表明数值模拟方法有效。另外还分析了结冰对机翼升力、阻力和压力系数的影响,其结果可以指导飞机机翼防／除冰系统的设计研究     

二维翼型大尺寸过冷水滴撞击特性及冰形分析

基于现有大尺寸过冷水滴(supercooled large droplet, SLD)动力学特性,分析水滴变形对阻力的影响.并根据几种典型的反弹/飞溅模型,分析了SLD的阻力变化、反弹、飞溅等对水滴撞击特性的影响,采用软件FENSAP-ICE的飞溅模型和LEWICE 2.0的反弹模型研究了反弹及飞溅现象对冰形的影响.计算结果显示:水滴撞击前的破碎现象对水滴尺寸分布有较大的影响,进行撞击特性以及冰形计算的时候需进行考虑;SLD破碎、飞溅、反弹降低了局部水收集系数、减小了水滴撞击范围;飞溅现象主要发生在机翼前缘附近区域,反弹主要在撞击边缘区域;水滴直径增加,飞溅现象逐渐减弱,但边缘位置的反弹现象一直很明显.SLD变形带来的阻力影响对冰形及结冰区域影响很小;与未考虑飞溅及反弹现象得到的冰形比较,考虑飞溅及反弹得到冰形前缘区域形状变化不大,但是整体结冰区域减小.      

基于润滑理论的二维积冰数值模拟

将基于润滑理论的水膜-冰层模型推广到在任意二维截面上建立的正交曲线坐标系,得到描述二维型线表面水膜流动和积冰的偏微分控制方程.采用一种隐式-显式有限差分格式建立控制方程组的代数形式,给出求解非稳态控制方程组的数值方法.为验证模型和数值解法的有效性,在典型的航空积冰和传输线积冰环境下对翼型和传输线表面的积冰算例进行数值模拟.将水膜-冰层模型的冰形计算结果与传统Messinger模型的模拟结果以及冰风洞试验结果进行对比,低温明冰条件下采用当前方法计算的翼型表面冰形接近于Messinger模型的模拟冰形曲线;相对高温条件下的计算结果比传统Messinger模型更为精确.低速积冰环境下Messinger模型难以模拟的传输线表面积冰同样可以采用水膜-冰层模型进行有效 预测.     

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.      

带整体式粒子分离器的涡轴发动机进口支板的三维积冰数值研究

整体式粒子分离器对涡轴发动机的气动乃至积冰都会有影响。为了获得涡轴发动机进口支板的积冰特性,以包含整体式粒子分离器的涡轴发动机进气机匣为模型,选取间断最大结冰条件,采用欧拉-欧拉法模拟了进气机匣内的空气-过冷水滴两相流场,并计算了支板表面的水滴撞击特性,再应用考虑水膜流动和蒸发的三维积冰模型对支板表面的积冰进行了模拟。计算结果表明,机匣进口的水滴有99.4%进入了扫气流道,而且结冰参数在支板前缘上游呈现出明显的周向不均匀性。对于主流道下游的4片支板,仅距离蜗壳起始位置最近的支板前缘局部受到显著的水滴撞击,最大水收集系数达到3.8,当积冰总时间为74s时,该支板表面最大积冰厚度约8mm,其余3片支板表面几乎没有水滴撞击和积冰现象。本文的研究结果可为考虑整体式粒子分离器影响的涡轴发动机进口支板的防冰设计提供依据。