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.     

Black Hole Studies: Overview and Outlook

In this article, I will attempt to give an overview of the motivations for studying black holes and of the current major problems in the field. I will also give some perspectives on what can be done in the future, focusing on instrumentation which has already been approved. This chapter will necessarily be more speculative than the other chapters in this volume.     

X-Ray Spectroscopy of Galaxy Clusters: Beyond the CIE Modeling

X-ray spectra of galaxy clusters are dominated by the thermal emission from the hot intracluster medium. In some cases, besides the thermal component, spectral models require additional components associated, e.g., with resonant scattering and charge exchange. The latter produces mostly underluminous fine spectral features. Detection of the extra components therefore requires high spectral resolution. The upcoming X-ray missions will provide such high resolution, and will allow spectroscopic diagnostics of clusters beyond the current simple thermal modeling. A representative science case is resonant scattering, which produces spectral distortions of the emission lines from the dominant thermal component. Accounting for the resonant scattering is essential for accurate abundance and gas motion measurements of the ICM. The high resolution spectroscopy might also reveal/corroborate a number of new spectral components, including the excitation by non-thermal electrons, the deviation from ionization equilibrium, and charge exchange from surface of cold gas clouds in clusters. Apart from detecting new features, future high resolution spectroscopy will also enable a much better measurement of the thermal component. Accurate atomic database and appropriate modeling of the thermal spectrum are therefore needed for interpreting the data.     

Observational Appearance of Black Holes in X-Ray Binaries and AGN

Accretion onto black holes powers most luminous compact sources in the Universe. Black holes are found with masses extending over an extraordinary broad dynamic range, from several to a few billion times the mass of the Sun. Depending on their position on the mass scale, they may manifest themselves as X-ray binaries or active galactic nuclei. X-ray binaries harbor stellar mass black holes—endpoints of the evolution of massive stars. They have been studied by X-ray astronomy since its inception in the early 60-ies, however, the enigma of the most luminous of them—ultra-luminous X-ray sources, still remains unsolved. Supermassive black holes, lurking at the centers of galaxies, are up to hundreds of millions times more massive and give rise to the wide variety of different phenomena collectively termed “Active Galactic Nuclei”. The most luminous of them reach the Eddington luminosity limit for a few billions solar masses object and are found at redshifts as high as z≥5–7. Accretion onto supermassive black holes in AGN and stellar- and (possibly) intermediate mass black holes in X-ray binaries and ultra-luminous X-ray sources in star-forming galaxies can explain most, if not all, of the observed brightness of the cosmic X-ray background radiation. Despite the vast difference in the mass scale, accretion in X-ray binaries and AGN is governed by the same physical laws, so a degree of quantitative analogy among them is expected. Indeed, all luminous black holes are successfully described by the standard Shakura-Sunyaev theory of accretion disks, while the output of low-luminosity accreting black holes in the form of mechanical and radiative power of the associated jets obeys to a unified scaling relation, termed as the “fundamental plane of black holes”. From that standpoint, in this review we discuss formation of radiation in X-ray binaries and AGN, emphasizing their main similarities and differences, and examine our current knowledge of the demographics of stellar mass and supermassive black holes.     

Measuring the Masses of Supermassive Black Holes

Supermassive black holes reside at the centers of most, if not all, massive galaxies: the difference between active and quiescent galaxies is due to differences in mass accretion rate and radiative efficiency rather than whether or not they have nuclear black holes. In this contribution, methods for measuring the masses of supermassive black holes are discussed, with emphasis on reverberation mapping which is most generally applicable to accreting supermassive black holes and, in particular, to distant quasars where time resolution can be used as a surrogate for angular resolution. Indirect methods based on scaling relationships from reverberation mapping studies are also discussed, along with their current limitations.     

航空发动机叶片气膜孔测量技术研究

基于航空发动机叶片冷却气膜孔的设计、加工和国家＂十一五＂计量科研项目的技术攻关及检测试验研究,本文简要介绍了叶片气膜孔位置度检测技术的思路、途径和方法,力求解决叶片气膜孔加工中的量值传递或溯源的难题,使我国在叶片等空间曲面小孔测量领域实现重大突破。     

The Influence of Black Hole Binarity on Tidal Disruption Events

Space Science Reviews - Interstellar dust from the Local Interstellar Cloud was detected unambiguously for the first time in 1992&nbsp;(Grün et&nbsp;al. in Nature 362:428–430,...     

企业信息化"黑洞"与精益管理

文章分析了企业信息化"黑洞"产生的深层次原因,提出了企业管理理念应与信息技术发展阶段相适应的观点,在此基础上引出了精益管理的概念,分析了精益管理对企业全面、成功实施信息化的重要作用.     

X射线法测试钛合金结构件残余应力的适用性研究

利用四点弯曲机加载的钛合金板材试样及高应力钛合金标样模拟结构件表面测试状态,研究X射线法测试复杂钛合金构件表面残余应力的适用性。结果表明:表面曲率及β角扫描范围对测试结果影响不显著;径向测试面倾角大于20°时测试重复性急剧变差,超过30°时结果不可使用,轴向测试面测试结果随倾角增大而减小,30°时减小超过20%。     

框架类远距离浅孔同轴度误差测量方法的探讨

讨论了利用三坐标测量机,测量框架类零件远距离浅孔同轴度误差的方法,分析了各种测量方法之间的区别,给出了一种适合框架类远距离浅孔公共轴线的测量方法.     

Measuring the Distribution of Ocean Mass Using GRACE

The Gravity Recovery and Climate Experiment (GRACE), which was successfully launched March 17, 2002, has the potential to create a new paradigm in satellite oceanography with an impact perhaps as large as was observed with the arrival of precision satellite altimetry via TOPEX/Poseidon (T/P) in 1992. The simulations presented here suggest that GRACE will be able to monitor non-secular changes in ocean mass on a global basis with a spatial resolution of ≈500 km and an accuracy of ≈3 mm water equivalent. It should be possible to recover global mean ocean mass variations to an accuracy of ≈1 mm, possibly much better if the atmospheric pressure modeling errors can be reduced. We have not considered the possibly significant errors that may arise due to temporal aliasing and secular gravity variations. Secular signals from glacial isostatic adjustment and the melting of polar ice mass are expected to be quite large, and will complicate the recovery of secular ocean mass variations. Nevertheless, GRACE will provide unprecedented insight into the mass components of sea level change, especially when combined with coincident satellite altimeter measurements. Progress on these issues would provide new insight into the response of sea level to climate change. This revised version was published online in August 2006 with corrections to the Cover Date.     

用自由空间法测量材料复介电常数的研究

分析电磁波在自由空间通过平板电介质材料的传播特性,得到了散射参数与复介电常数之间的关系式和求解复介电常数的三种表达式,并对三种表达式分别进行误差分析.解决自由空间法测量电介质材料复介电常数的不稳定性问题和相位模糊性问题.建立测试系统,并在X波段对平板电介质材料进行测量.实验结果表明,本测试方法和测试系统是正确的.     

基于遥测技术的发动机涡轮转子叶片动应力测量

根据某型发动机涡轮叶片动应力测量试验要求,提出了一种基于遥测技术的高温动应力测量系统方案,并重点介绍了测量系统组成、工作原理及系统标定。利用该测量系统,成功获取了发动机涡轮叶片动应力数据。整个试验过程中,遥测系统工作正常,表现出良好的冷却效果、电源稳定性和信号频率跟随性。试验结果表明,该型发动机在特定转速区间内存在窄频带共振,振幅水平较高,具有明显的破坏性,结果可信。     

图像模板测量技术在零件不规则薄圆孔检测中的应用

针对不规则薄圆孔的检测,提出了一种基于数字图像处理的模板匹配检测方法,运用数字图像处理技术对采集的圆孔图像进行截取、降噪、分割、边缘检测等处理,再把提取出的圆与标定模板上的标准圆进行比较,实现对不规则圆孔尺寸的检测,并通过实验证明了该方法的可行性和实用性。     

基于轮廓法测试铝合金拉弯成形残余应力研究

以2026-T3511铝合金T形结构件的拉弯成形件为研究对象,首先采用线切割将T形结构件分割成两块具有T形截面的试样,然后基于轮廓法测试应力原理应用激光位移传感器分别测试两个分割截面的轮廓变化,进而将两个截面的测量值拟合平均后与有限元模型结合以计算该试样的初始残余应力,从而获得该T形结构件的横截面法向应力并分析其分布特征。研究结果表明,基于轮廓法测得的应力分布与有限元仿真结果分布规律相近:峰值压应力为60MPa,峰值拉应力为40MPa;轮廓法在航空结构件应力测试中能够准确地获得其他测试方法无法获得的横截面完整的应力分布。     

利用Delphi设计开发卫星测控设备远程实时监控子系统

介绍了卫星某频段控制设备远程实时监控系统的总体设计思想,以及利用Ｄｅｌｐｈｉ３ ．０ 开发的具体实现方法,其中涉及了许多Ｄｅｌｐｈｉ 的最新技术。