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.     

Time-resolved spectroscopy of accretion disks in Algols

Time-resolved spectroscopy during the eclipse of short-period Algol systems, has shown their accretion disks to be small, turbulent structures with non-Keplerian velocity fields and asymmetries between the leading and trailing sides of the disk. These transient disks are produced by the impact of the gas stream on the mass-gaining star, and occur in systems where the star is just large enough to ensure the stream collision is complete. These emission line disks and the excess continuum emission do not always occur together. The permanent accretion disks in at least a few of the long-period Algol systems have features in common with the transient disks including non-Keplerian velocity fields.     

Time-resolved spectroscopy of accretion disks in Algols

Time-resolved spectroscopy during the eclipse of short-period Algol systems, has shown their accretion disks to be small, turbulent structures with non-Keplerian velocity fields and asymmetries between the leading and trailing sides of the disk. These transient disks are produced by the impact of the gas stream on the mass-gaining star, and occur in systems where the star is just large enough to ensure the stream collision is complete. These emission line disks and the excess continuum emission do not always occur together. The permanent accretion disks in at least a few of the long-period Algol systems have features in common with the transient disks including non-Keplerian velocity fields.     

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.     

Theoretical modelling of Algol disks

A brief review of various theoretical approaches to model accretion disks is presented. Emphasis is given to models that determine self-consistently the structure of a disk together with the radiation field. It is argued that a proper treatment of the vertical structure is essential for calculating theoretical spectra to be compared with observations. In particular, it is shown that hot layers above an accretion disk (sometimes called disk “chromospheres” or “coronae”), whose presence is indicated by recent UV observations of strong emission lines of highly ionized species, may be explained using simple energy balance arguments.     

Observational Constraints on Transport (and Mixing) in Pre-Main Sequence Disks

Currently available observational constraints on transport mechanisms in pre-main sequence disks are reviewed. The main observable quantity accessable by imaging the spatial structure of disks is the mass accretion rate, which constrains angular momentum transport, and migration and diffusion of disk material. This revised version was published online in June 2006 with corrections to the Cover Date.     

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.     

Nucleosynthesis from non-thermal particles

The long-standing problem of nucleosynthesis from non-thermal charged particles is reviewed with emphasis on some novel points. Recent theoretical results predict very efficient acceleration of nuclei (up to GeV range) by violent systems with energy release in the form of multiple shock waves —OB associations and coronae of AGNs and black holes candidates in galactic accretion disks. A detection of gamma-line emission from the Orion complex by theCOMPTEL telescope on board ofGRO could confirm theoretical predictions. Production of lithium by non-thermal particles in Orion-like objects is discussed. The mechanism can be responsible for the observed variations of abundance of isotopes.     

Photometric effects of accretion disks in long-period eclipsing binaries

Summary A multi-year photometric program on long-period eclipsing binaries has begun to uncover some properties of accretion disks in these systems. Emission and transmission properties can sometimes be found from light curve features produced by partial eclipses of the disk by the cool star, and by partial occultations of the cool star by the disk. These disks do not have the classical alpha structure. They are optically thin normal to the orbital plane, but may be geometrically thicker than purely gravitationally-stratified disks. Disk gas may be contaminated by dust particles acquired from the outer layers of the cool loser. In some systems, high states, produced by elevated mass accretion by the hot star, occur, suggesting that the mass distribution in the disk is clumpy. However mass-transfer rates are found, they lie between 10^-7 and 10^-6 solar masses per year.While this binary sample is small at the moment, some of its properties are shared with other systems. The author has five-color observations of about a dozen additional systems, which may fill out this picture more fully.     

计入离心力影响的直升机旋翼翼型结冰数值模拟

建立了一套计入离心力影响的直升机旋翼翼型结冰的数值模拟方法.首先生成围绕翼型的贴体正交网格,然后用Navier-Stokes（N-S）方程求解黏性绕流流场.在此基础上,利用拉格朗日法建立水滴运动方程.其中,为提高计算效率,提出了结合位移矢量的水滴所处单元寻觅方法.最后,结合桨叶工作特点,发展了一种计入离心力影响的三维结冰模型.通过与桨叶结冰实验的对比,验证了本文结冰预测方法的可靠性.对比常规结冰模型,桨叶结冰量减少22.3%;若考虑桨叶的挥舞运动影响,桨叶结冰量进一步减少,表明了离心力及桨叶运动在结冰数值模拟中的重要性.通过不同剖面间的结冰量和冰形对比,分析并获得了桨叶结冰特征.结果表明离心力的影响程度随径向位移的增加而增加,下翼面结冰量随挥舞角的增加而减少.      

Alfvén waves in the context of solar-like star formation: accretion columns and disks

In this work we examine the damping of Alfvén waves as a source of plasma heating in disks and magnetic funnels of young solar like stars, the T Tauri stars. We apply four different damping mechanisms in this study: viscous-resistive, collisional, nonlinear and turbulent, exploring a wide range of wave frequencies, from 10⁻⁵Ω_i to 10⁻¹Ω_i (where Ω_i is the ion-cyclotron frequency). The results show that Alfvénic heating can increase the ionization rate of accretion disks and elevate the temperature of magnetic funnels of T Tauri stars opening possibilities to explain some observational features of these objects. This revised version was published online in August 2006 with corrections to the Cover Date.     

Accretion onto Magnetic White Dwarfs

The standard model of stationary and time-dependent accretion onto magnetic white dwarfs are reviewed, with emphasis on the hydrodynamic structure and the emission properties of the post-shock flow. Observational consequences and applications of the model are discussed, and results obtained from our recent calculations are also presented.     

Theoretical modelling of Algol disks

A brief review of various theoretical approaches to model accretion disks is presented. Emphasis is given to models that determine self-consistently the structure of a disk together with the radiation field. It is argued that a proper treatment of the vertical structure is essential for calculating theoretical spectra to be compared with observations. In particular, it is shown that hot layers above an accretion disk (sometimes called disk chromospheres or coronae), whose presence is indicated by recent UV observations of strong emission lines of highly ionized species, may be explained using simple energy balance arguments.1987–88 JILA Visiting Fellow.This work was in part supported by a NASA grant ADP U-003-88 (Plavec and Hubeny). I also wish to thank the organizers of the IAU Colloquium 107 for the travel grant which enabled me to attend the meeting.     

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.      

具有非线性摩擦阻尼随机失谐的叶盘系统响应特性

针对目前含非线性摩擦阻尼失谐叶盘系统振动局部化机理研究存在的诸多困难,尤其是其非线性力学模型的建立和求解等难题.建立了具有滞迟干摩擦阻尼随机失谐的叶盘系统力学模型,并利用增量谐波平衡法分析了叶盘系统干摩擦力失谐度、耦合强度、黏性阻尼比和摩擦力强度等系统参数对叶盘系统受迫响应的影响规律.研究表明:含非线性摩擦阻尼的谐调叶...     

Planetesimals and Satellitesimals: Formation of the Satellite Systems

The origin of the regular satellites ties directly to planetary formation in that the satellites form in gas and dust disks around the giant planets and may be viewed as mini-solar systems, involving a number of closely related underlying physical processes. The regular satellites of Jupiter and Saturn share a number of remarkable similarities that taken together make a compelling case for a deep-seated order and structure governing their origin. Furthermore, the similarities in the mass ratio of the largest satellites to their primaries, the specific angular momenta, and the bulk compositions of the two satellite systems are significant and in need of explanation. Yet, the differences are also striking. We advance a common framework for the origin of the regular satellites of Jupiter and Saturn and discuss the accretion of satellites in gaseous, circumplanetary disks. Following giant planet formation, planetesimals in the planet’s feeding zone undergo a brief period of intense collisional grinding. Mass delivery to the circumplanetary disk via ablation of planetesimal fragments has implications for a host of satellite observations, tying the history of planetesimals to that of satellitesimals and ultimately that of the satellites themselves. By contrast, irregular satellites are objects captured during the final stages of planetary formation or the early evolution of the Solar System; their distinct origin is reflected in their physical properties, which has implications for the subsequent evolution of the satellites systems.     

EXOSAT observations of the X-ray pulsar 4U1145-619

EXOSAT observations of the X-ray pulsar 4U1145-619 during June and July 1983 and July 1984 confirm that this source shows a regular 187 day outburst cycle in X-rays. The results from pulse timing and X-ray spectroscopy are discussed in terms of a model for 4U1145-619 involving an eccentric binary system in which there is variable accretion from the Be primary star onto a companion neutron star.     

飞机机翼表面霜状冰结冰过程的数值模拟

提出了一种处理结冰后结冰表面固壁区域移动的移动边界技术,结合欧拉坐标系下空气-过冷水滴两相流动控制方程的计算,对霜状冰的结冰过程进行了数值模拟,得到了NACA0012机翼在0°和4°攻角下机翼表面结冰后形成的冰形,与文献中的实验数据对比,表明本文的方法是可行和有效的。      

基于Myers模型的三维结冰数值仿真

三维结冰表面上的水膜流动和结冰增长是结冰计算模型应考虑的核心内容,其中广泛应用的是Myers模型。Myers模型考虑了空气剪切力和空气压力对结冰表面水膜流动的影响,以及冰层、水膜和空气之间的导热与对流传热对结冰速率的影响。本文在使用Myers模型进行结冰预测时,发现Myers模型对霜冰转化为明冰的判断标准存在缺陷,会在结冰极限处产生不合理的冰角。因此对Myers模型的结冰类型判断标准进行了修改,对机翼表面的结冰过程进行了更加准确的模拟,并应用了有效的离散算法计算水膜流动和结冰增长过程。对比了二维NACA0012翼型的单步法、多步法计算结果和实验结果。明冰结冰温度较低时,本文计算结果与实验结果吻合很好,明冰结冰温度较高时,本文对上冰角的计算与实验结果有一定差距。本文提供了三维GLC-305后掠翼的结冰计算结果和实验结果的对比,冰角厚度的计算结果略小于实验结果,但整体趋势一致。     

发动机进气道短舱前缘结冰三维模拟研究

为计算发动机进气道短舱前缘的结冰冰形,在Messinger结冰热力学模型的基础上发展了一套纯三维的表面溢流水流动结冰模型。考虑空气摩擦力为表面溢流水流动的主要驱动力,用空气对进气道表面的剪切力来确定溢流水的流动方向及流量分配。为求解溢流水结冰模型,发展了一套重复查找表面控制体状态的方法,能够快速完成整个三维表面的计算。用该方法对某三维发动机进气道进行计算,得到了三维结冰冰形,并将计算结果与FENSAP-ICE计算结果进行了对比,结果显示两者的冰形轮廓基本一致,仅在冰角处存在差异,表明本文三维发动机结冰计算模型与计算方法是有效的,其计算精度与FENSAP-ICE结果相当。