Black Hole Spin via Continuum Fitting and the Role of Spin in Powering Transient Jets

The spins of ten stellar black holes have been measured using the continuum-fitting method. These black holes are located in two distinct classes of X-ray binary systems, one that is persistently X-ray bright and another that is transient. Both the persistent and transient black holes remain for long periods in a state where their spectra are dominated by a thermal accretion disk component. The spin of a black hole of known mass and distance can be measured by fitting this thermal continuum spectrum to the thin-disk model of Novikov and Thorne; the key fit parameter is the radius of the inner edge of the black hole’s accretion disk. Strong observational and theoretical evidence links the inner-disk radius to the radius of the innermost stable circular orbit, which is trivially related to the dimensionless spin parameter a _? of the black hole (|a _?|<1). The ten spins that have so far been measured by this continuum-fitting method range widely from a _?≈0 to a _?>0.95. The robustness of the method is demonstrated by the dozens or hundreds of independent and consistent measurements of spin that have been obtained for several black holes, and through careful consideration of many sources of systematic error. Among the results discussed is a dichotomy between the transient and persistent black holes; the latter have higher spins and larger masses. Also discussed is recently discovered evidence in the transient sources for a correlation between the power of ballistic jets and black hole spin.     

Multi-Wavelength Variability

Multiwavelength variability data, combined with spectral-timing analysis techniques, provides information about the causal relationship between different physical components in accreting black holes. Using fast-timing data and long-term monitoring, we can probe the behaviour of the same components across the black hole mass scale. In this chapter we review the observational status of multiwavelength variability in accreting black holes, from black hole X-ray binaries to AGN, and consider the implications for models of accretion and ejection, primarily considering the evidence for accretion disc and jet variability in these systems. We end with a consideration of future prospects in this quickly-developing field.     

Current Status of Simulations

As the title suggests, the purpose of this chapter is to review the current status of numerical simulations of black hole accretion disks. This chapter focuses exclusively on global simulations of the accretion process within a few tens of gravitational radii of the black hole. Most of the simulations discussed are performed using general relativistic magnetohydrodynamic (MHD) schemes, although some mention is made of Newtonian radiation MHD simulations and smoothed particle hydrodynamics. The goal is to convey some of the exciting work that has been going on in the past few years and provide some speculation on future directions.     

Fast Variability from Black-Hole Binaries

Currently available information on fast variability of the X-ray emission from accreting collapsed objects constitutes a complex phenomenology which is difficult to interpret. We review the current observational standpoint for black-hole binaries and survey models that have been proposed to interpret it. Despite the complex structure of the accretion flow, key observational diagnostics have been identified which can provide direct access to the dynamics of matter motions in the close vicinity of black holes and thus to the some of fundamental properties of curved spacetimes, where strong-field general relativistic effects can be observed.     

Searching for Black Holes in Space

Although General Relativity had provided the physical basis of black holes, evidence for their existence had to await the Space Era when X-ray observations first directed the attention of astronomers to the unusual binary stars Cygnus X-1 and A0620-00. Subsequently, a number of faint Ariel 5 and Uhuru X-ray sources, mainly at high Galactic latitude, were found to lie close to bright Seyfert galaxies, suggesting the nuclear activity in AGN might also be driven by accretion in the strong gravity of a black hole. Detection of rapid X-ray variability with EXOSAT later confirmed that the accreting object in an AGN is almost certainly a supermassive black hole.     

Scaling Relations from Stellar to Supermassive Black Holes

Accretion is a ubiquitous phenomenon—it is seen in sources ranging from young stars to accreting supermassive black holes in the centres of galaxies. Here, we present the known empirical connections between stellar mass X-ray binaries and active galactic nuclei. We argue that this implies that both the accretion disc and the jet are scale invariant with respect to the black hole mass. Finally, we show that also accretion discs and jets in sources with a different accretor can be connected empirically to accreting black holes, hinting towards a common mechanism of accretion in all sources.     

Effect of turbulence models on predicting convective heat transfer to hydrocarbon fuel at supercritical pressure

A variety of turbulence models were used to perform numerical simulations of heat transfer for hydrocarbon fuel flowing upward and downward through uniformly heated vertical pipes at supercritical pressure. Inlet temperatures varied from 373 K to 663 K, with heat flux rang-ing from 300 kW/m2 to 550 kW/m2. Comparative analyses between predicted and experimental results were used to evaluate the ability of turbulence models to respond to variable thermophys-ical properties of hydrocarbon fuel at supercritical pressure. It was found that the prediction per-formance of turbulence models is mainly determined by the damping function, which enables them to respond differently to local flow conditions. Although prediction accuracy for experimental results varied from condition to condition, the shear stress transport (SST) and launder and sharma models performed better than all other models used in the study. For very small buoyancy-influenced runs, the thermal-induced acceleration due to variations in density lead to the impairment of heat transfer occurring in the vicinity of pseudo-critical points, and heat transfer was enhanced at higher temperatures through the combined action of four thermophysical properties: density, viscosity, thermal conductivity and specific heat. For very large buoyancy-influenced runs, the thermal-induced acceleration effect was over predicted by the LS and AB models.     

Numerical simulation of gas dynamics and heat exchange of jet impinging on a surface

The results of verification calculation of single jets impinging on a pedestal are presented; the result of calculations is evaluation of the local Nusselt numbers and flow gas-dynamic characteristics. On the basis of literature analysis we picked out several turbulence models to close the system of equations. The calculation results are compared with the known experimental data. It is shown, that only the v ² ? f turbulence model allows the augmented turbulence characteristics to be predicted adequately that correspond to a change of the flow conditions at short jet-to-surface distances. All models being investigated except the Spalart-Allmaras model show satisfactory agreement both in the stagnation region and in the near-wall jet zone.     

Modelling Spectral and Timing Properties of Accreting Black Holes: The Hybrid Hot Flow Paradigm

The general picture that emerged by the end of 1990s from a large set of optical and X-ray, spectral and timing data was that the X-rays are produced in the innermost hot part of the accretion flow, while the optical/infrared (OIR) emission is mainly produced by the irradiated outer thin accretion disc. Recent multiwavelength observations of Galactic black hole transients show that the situation is not so simple. Fast variability in the OIR band, OIR excesses above the thermal emission and a complicated interplay between the X-ray and the OIR light curves imply that the OIR emitting region is much more compact. One of the popular hypotheses is that the jet contributes to the OIR emission and even is responsible for the bulk of the X-rays. However, this scenario is largely ad hoc and is in contradiction with many previously established facts. Alternatively, the hot accretion flow, known to be consistent with the X-ray spectral and timing data, is also a viable candidate to produce the OIR radiation. The hot-flow scenario naturally explains the power-law like OIR spectra, fast OIR variability and its complex relation to the X-rays if the hot flow contains non-thermal electrons (even in energetically negligible quantities), which are required by the presence of the MeV tail in Cyg X-1. The presence of non-thermal electrons also lowers the equilibrium electron temperature in the hot flow model to ?100 keV, making it more consistent with observations. Here we argue that any viable model should simultaneously explain a large set of spectral and timing data and show that the hybrid (thermal/non-thermal) hot flow model satisfies most of the constraints.     

非线性 k-ε 紊流模型在平面叶栅紊流计算中的应用

 采用Speziale的非线性k-ε模型计算了平面叶栅内的紊流流动,并且与标准的k-ε模型的计算结果作了对比,表明非线性模型同样可以应用于具有周期性边界条件的复杂流动,在紊流量的计算结果上表现出了明显的各向异性。     

Observational Tests of the Picture of Disk Accretion

In this chapter, I present a summary of observational tests of the basic picture of disk accretion. An emphasis is placed on tests relevant to black holes, but many of the fundamental results are drawn from studies of other classes of systems. Evidence is discussed for the basic structures of accretion flows. The cases of systems with and without accretion disks are discussed, as is the evidence that disks actually form. Also discussed are the hot spots where accretion streams impact the disks, and the boundary layers in the inner parts of systems where the accretors are not black holes. The nature of slow, large amplitude variability is discussed. It is shown that some of the key predictions of the classical thermal-viscous ionization instability model for producing outbursts are in excellent agreement with observational results. It is also show that there are systems whose outbursts are extremely difficult to explain without invoking variations in the rate of mass transfer from the donor star into the outer accretion disk, or tidally induced variations in the mass transfer rates. Finally, I briefly discuss recent quasar microlensing measurements which give truly independent constraints on the inner accretion geometry around black holes.     

涡轮导向叶栅通道内紊流特性的实验研究

本文对一种高压涡轮导向叶栅中的紊流特性进行了实验研究。在雷诺数为100000的工况下, 采用二维热线对叶栅通道内垂直于叶高的平面内的平均速度, 脉动速度, 及雷诺切应力相关系数进行测量。并结合以前通过五孔针测量取得的流场进行了分析, 得出了该叶栅中紊流参数的变化规律。实验结果表明: 叶栅端壁区的紊流流动, 基本保持各向同性; 通道涡和马蹄涡内存在高紊流度和雷诺切应力的紊流核心。本实验结果为分析研究叶栅端壁换热特性奠定了基础。      

隐式紧耦合SST和TNT湍流模型的高速流动数值模拟

将SST(shear stress transport)和TNT(turbulent/non-turbulent)湍流模型输运方程与平均流场控制方程进行隐式紧耦合求解,结合当地时间步长方法和湍流源项隐式处理确保求解过程的快速和稳定.采用AUSMPW+(AUSM by pressure-based weight functions)格式和LU-SGS(lower-upper symmetric Gauss-Seidel)隐式紧耦合方法对高超声速压缩拐角流动、锥柱裙流动和超声速非对称激波/边界层干扰问题进行了数值模拟.计算结果与实验值的对比表明:SST模型和TNT湍流模型可以很好地预测15°压缩拐角流动的壁面压力和热流密度;随着压缩拐角的增大,计算结果与实验值偏差增大;可压缩性修正对压缩拐角流动的压力和热流密度分布有很大影响,对超声速非对称激波/边界层干扰流动影响很小;隐式紧耦合方法比显式紧耦合方法具有更好的收敛特性.      

涡轮导叶W型孔全气膜冷却效率实验研究

为了研究涡轮导叶W型孔全气膜冷却效率的分布规律,使用热色液晶测量了在流量比为5.5%、8.4%和12.5%,主流湍流度为1%、9%和15%下W型孔全气膜涡轮导叶的气膜冷却效率,并与相同工况下的圆柱型孔全气膜叶片的冷却效率结果进行了对比。结果表明：在低湍流度下,流量比变化对W型孔叶片不同区域冷却效率的影响规律不同;而在高湍流度下,流量比增大使W型孔叶片的冷却效率整体升高;在本文研究的所有流量比下,W型孔叶片的冷却效率均随着湍流度的升高而降低;与圆柱型孔叶片相比,在中低湍流度下,W型孔的冷气壁面贴附性和展向覆盖效果更好,W型孔叶片的冷却效率具有明显优势,然而在高湍流度下由于W型孔的冷气速度低且分布分散,易在高湍流度影响下耗散,W型孔叶片的冷却效率优势较小,甚至在高湍流度大流量比下,圆柱型孔叶片的面平均冷却效率比W型孔叶片高15%左右。     

平行平板内连续布置肋块流场与传热的数值模拟

为了研究平行平板内连续布置8个肋块的流场结构和传热现象, 利用计算流体力学软件FLU-ENT6.2内置的标准k-ε湍流模型、RNGk-ε湍流模型和Realizablek-ε湍流模型对此进行了数值模拟并对结果作了比较.流场结果显示在相同来流条件下, 由Realizablek-ε模型预测的肋块间逆时针方向回流区最大, 标准k-ε模型最小.数值结果表明从第2个肋块开始加热段表面压力系数Cp和努塞尔数Nu开始呈周期性变化.同时将第7个肋表面的努塞尔数数值解与实验值进行了比较, 结果为三种湍流模型都能准确模拟出努塞尔数的变化趋势.计算结果可为工程设计和使用提供参考.      

复杂积冰翼型气动性能分析

为了克服复杂外形难以划分结构化网格的问题, 采用结构/非结构混合多块网格对复杂积冰翼型的气动性能-进行了分析计算.在靠近积冰边界的内层采用了非结构网格, 在非结构网格外采用结构化网格以节省存储空间和计算时间.不同类型网格之间采用了点点对接的方式以简化通量重构的处理方式.整个流动区域采用SST湍流模型, 求解了雷诺平均N-S方程.数值计算结果表明结构/非结构混合多块网格在复杂积冰翼型气动性能计算上的可行性, 积冰对翼型的气动性能造成了严重的影响.      

湍流大涡数值模拟进展

本文简要陈述湍流大涡数值模拟的原理、优点,着重讨论湍流大涡数值模拟方法的关键问题及其可能解决的途径,包括脉动的过滤、亚格子模型、近壁模型和标量湍流的大涡数值模拟中的特殊问题.文章强调大涡数值模拟中亚格子应力的本质是可解尺度湍流和不可解尺度湍流动量间的输运,并以作者最近提出的新型亚格子模型说明发展亚格子模型的正确途径.文章最后提出湍流大涡数值模拟近期需要迫切解决的问题和其他具有挑战性的方向.     

Magnetic energy release near accreting black holes

The observed non-thermal emission from accreting compact objects is often understood in terms of the expected magnetic activity of accretion disks. This review discusses the constraints on this view point that can be obtained from, principally, the X-ray spectra and the X-ray variability of black hole candidates.Furthermore, the traditional view of an accretion disk corona, put forward as the source of the non-thermal emission, analogous to the solar corona is shown to be wrong on a few important points. Firstly, the density in the equilibrium accretion disk corona is extremely low. A reasonable plasma density is retained by pair production processes similar to those existing in the pulsar magnetosphere. Secondly, the dominant resistivity in the accretion the disk on the current carrying electrons.     

孔间距和前倾角对进出口扩张形气膜孔流量系数的影响(英文)

Discharge coefficients of 3-in-1 hole of three inclination angles and three spacing between holes are presented which described the discharge behavior of a row of holes. The inlet and outlet of the 3-in-1 hole both have a 15° lateral expansion. The flow conditions considered are mainstream turbulence intensities and density ratios of secondary flow to mainstream. The momentum flux ratios varied in the range from 1 to 4. The comparison is made of the discharge coefficients of three shaped holes to find an optimal hole with low flow loss. The results show that the discharge coefficients of 3-in- 1 hole are highest in three shaped holes and therefore this article is focused on the measurements of discharge coefficients of 3-in-1 hole for various geometries and aerodynamic parameters. The measured results of 3-in-1 hole indicate that turbulence intensities, density ratios and momentum flux ratios have weak influence on discharge coefficients for inclination angle of 20°. The high turbulence intensity yields the small discharge coefficients for inclination angle of 45° and 90°. The increased both momentum flux ratios and density ratios lead to the increased discharge coefficients for inclination angle of 45° and 90°. The increased inclination angle causes the rapidly increased discharge coefficients. There is a weak dependence of discharge coefficients on hole pitches.