Black hole spectral states and physical connections

The dramatic changes seen in the X-ray spectral and timing properties of accreting black hole candidates (BHCs) provide important clues about the accretion and jet formation processes that occur in these systems. Dividing the different source behaviors into spectral states provides a framework for studying BHCs. To date, there have been three main classification schemes with Luminosity-based, Component-based, or Transition-based criteria. The canonical, Luminosity-based criteria and physical models that are based on this concept do not provide clear explanations for several phenomena, including hysteresis of spectral states and the presence of jets. I discuss the re-definitions of states, focusing on an application of the Component-based states to more than 400 RXTE observations of the recurrent BHC 4U 1630–47. We compare the X-ray properties for the recent 2002–2004 outburst to those of an earlier (1998) outburst, during which radio jets were observed. The results suggest a connection between hysteresis of states and major jet ejections, and it is possible that both of these are related to the evolution of the inner radius of the optically thick accretion disk.     

Neutrino flares from black hole coronae

We present a model for neutrino flares in accreting black holes based on the injection of a non-thermal population of relativistic particles in a magnetized corona. The most important products of hadronic and photohadronic interactions at high energies are pions. Charged pions decay into muons and neutrinos; muons also decay yielding neutrinos. Taking into account these effects, coupled transport equations are solved for all species of particles and the neutrino production is estimated for the case of accreting galactic black holes.     

Constraining the mass of the black hole GX 339-4 using spectro-temporal analysis of multiple outbursts

We carried out spectro-temporal analysis of the archived data from multiple outbursts spanning over the last two decades from the black hole X-ray binary GX 339-4. In this paper, the mass of the compact object in the X-ray binary system GX 339-4 is constrained based on three indirect methods. The first method uses broadband spectral modelling with a two component flow structure of the accretion around the black hole. The broadband data are obtained from RXTE (Rossi X-ray Timing Explorer) in the range 3.0 to 150.0?keV and from Swift and NuSTAR (Nuclear Spectroscopic Telescope Array) simultaneously in the range 0.5 to 79.0?keV. In the second method, we model the time evolution of Quasi-periodic Oscillation (QPO) frequencies, considering it to be the result of an oscillating shock that radially propagates towards or away from the compact object. The third method is based on scaling a mass dependent parameter from an empirical model of the photon index ($\mathrm{\Gamma }$) – QPO ($\nu$) correlation. We compare the results at 90 percent confidence from the three methods and summarize the mass estimate of the central object to be in the range $8.28–11.89M_{\odot }$.     

SLX 1746-311 in outburst

We report on RXTE-PCA observations of SLX 1746-311 during a 100 day outburst in April 2003. We present the 3–20 keV PCA energy spectra of the source and study evolution of spectral parameters. The burst spectrum is soft with T_in 1.3 keV at the beginning of the outburst. There is a clear evidence of a hard power law component throughout the outburst. There is also an indication of a broad iron line. The source exhibits three state transitions with considerable change in the hardness ratio at low count rates. We discuss the possible scenario under which this unusual behaviour can be explained.     

X-ray observations of black-hole accretion disks

Our current theoretical and observational understandings of the accretion disks around Galactic black-holes are reviewed. Historically, a simple phenomenological accretion disk model has been used to interpret X-ray observations. Although such a phenomenological interpretation is still useful, high quality X-ray data from contemporary instruments allow us to test more realistic accretion disk models. In a simple and ideal case, the standard optically thick accretion disk model is successful to explain observations, such that the inner disk radius is constant at three times the Schwarzschild radius over large luminosity variations. However, when disk luminosity is close to or exceeds the Eddington luminosity, the standard disk model breaks, and we have to consider the “slim disk” solution in which radial energy advection is dominant. Recent observations of Ultra-luminous X-ray sources (ULXs), which may not be explained by the standard disk model, strongly suggest the slim disk solution. We compare theoretical X-ray spectra from the slim disk with observed X-ray spectra of ULXs. We have found that the slim disk model is successful to explain ULX spectra, in terms of the massive stellar black-holes with several tens of solar mass and the super-Eddington mass accretion rates. In order to explain the large luminosities (>10⁴⁰ ergs s⁻¹) of ULXs, “intermediate black-holes” (>100M) are not required. Slim disks around massive stellar black-holes of up to several tens of solar mass would naturally explain the observed properties of ULXs.     

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.     

一种非仿射高超声速飞行器的智能控制方法

针对非仿射高超声速飞行器控制问题，提出了一种基于强化学习的非线性反步控制方法。首先，基于高超声速飞行器的非仿射模型，设计了基于反步法的鲁棒跟踪控制器；其次，鉴于该控制器的性能和鲁棒性对参数比较敏感，借助深度确定性策略梯度的智能控制方法，对控制器进行了参数在线调整和控制指令补偿；最后，通过理论分析和仿真结果验证了当存在额外扰动和未建模动态时，所提出的智能控制器仍能保证攻角稳健跟踪期望目标。     

航天用时间触发网络系统同步性的故障分析

确定性网络的同步性在航天电子系统中至关重要。为保证确定性网络在发生故障的情况下也能正常的进行时间同步,本文采用spaceVPX标准中典型的双星拓扑交换结构配置基于时间触发以太网协议的可容错系统。针对此架构,使用以太网的航天系统中发生故障的单容错结构进行了仿真,模拟了几种时间同步协议控制帧异常的情况：协议控制帧包括冷启动帧、冷启动应答帧、集成帧从故障交换机的端口发送到网络中的一个终端系统后对于时间触发网络的同步网络所产生的影响。仿真结果表明,故障交换机会逐渐延长处于正常工作的终端系统的启动时间,进而不利于整个确定网络系统的同步过程,但是如果设置不同协议控制帧的周期超过一定的数值后,单点故障不会影响双冗余系统的启动时间。     

Relativistic jets from black hole binaries

Relativistic jets are now believed to be a fairly ubiquitous property of accreting compact objects, and are intimately coupled with the accretion history. Associated with rapid changes in the accretion states of the binary systems, ejections of relativistic plasma can be observed at radio frequencies on timescale of weeks before becoming undetectable. However, recent observations point to long term effects of these ejecta on the interstellar medium with the formation of large scale relativistic jets around binary systems.     

粒子滤波及其在航天器交会对接相对导航中的应用

在全面分析粒子滤波原理的基础上,提出一种改进高斯粒子滤波方法.该方法利用确定性采样滤波算法进行时间更新,替代高斯粒子滤波算法中的随机采样过程;另外,针对厚尾噪声情况,利用鲁棒统计方法对确定性采样滤波方法进行鲁棒性改进,并将其应用于所提出的改进高斯粒子滤波.将粒子滤波算法应用于交会对接相对导航问题,仿真结果表明,在多种测量噪声情况下,改进高斯粒子滤波较其他粒子滤波,能够在不过多损失估计精度的同时有效降低计算量.文中的研究成果为将粒子滤波应用于航天器导航问题提供了理论参考.     

Optical/X-ray correlations as a signature of jet-disc coupling in the accreting black hole XTE J1118+480

We interpret the rapid correlated UV/optical/X-ray variability of XTE J1118+480 as a signature of the coupling between the X-ray corona and a jet emitting synchrotron radiation in the optical band. We propose a scenario in which the jet and the X-ray corona are fed by the same energy reservoir where large amounts of accretion power are stored before being channelled into either the jet or the high energy radiation. This time-dependent model reproduces the main features of the rapid multi-wavelength variability of XTE J1118+480. A strong requirement of the model is that the total jet power should be at least a few times larger than the observed X-ray luminosity, implying a radiative efficiency for the jet _j  3 × 10⁻³. This would be consistent with the overall low radiative efficiency of the source. We present independent arguments showing that the jet probably dominates the energetic output of all accreting black holes in the low-hard state.     

三维CT重建几何参数的非线性最小二乘估计

重建几何参数的精度是3D-CT(Three Dimensional Computed Tomography)重建中严格控制的指标,在实际的X射线扫描成像中,这些参数无法直接测量得到,从而难以保证其精度.介绍了利用非线性最小二乘估计Feldkamp三维重建几何参数的方法,根据空间质点质心的投影位置与其投影的质心位置重合的原理,通过计算空间质点(实验中采用近似质点的目标体)投影质心坐标,求解非线性方程组估计重建几何参数的最优解.计算机模拟结果表明,在参数向量初始值接近于真值的情况下,估计所得参数值有较好的精度和重复性.利用此方法估计所得实际扫描系统的几何参数值进行三维重建,也得到了很好的重建结果.     

一种飞机大尺寸曲面测量点差异性规划方法

数字化测量技术在飞机大尺寸零部件检测的应用日益广泛，合理规划测量点数量和分布以精确地描述待测特征已成为关键问题之一。针对复杂曲线曲面的测量点规划问题，提出了一种基于确定性表达的测量点差异性规划方法。利用非均匀有理B样条（NURBS）理论精确拟合自由曲线，通过粒子群优化算法综合优化控制点及权因子，构建高精度的拟合曲线。提出了面向曲率特性和测量不确定度的布点策略，结合曲面特性建立完整、高效的测量点规划流程。基于CAA模块程序化实现了测量点规划方法，并以试验件为验证对象，验证了所提方法的可行性和系统的有效性。      

基于非线性神经网络的摆式列车检测系统动态补偿方法研究

针对零极点匹配动态补偿方法的不足 ,提出基于非线性神经网络的摆式列车检测系统动态补偿方法。根据陀螺平台实测超高数据 ,采用LM算法对所设计的非线性神经网络进行训练。仿真结果表明 ,所设计的神经网络动态补偿器能有效改善陀螺平台系统的动态特性 ,满足摆式列车倾摆控制实时性的要求。     

非线性随机动态系统学习建模方法

在动态神经网络及扩展卡尔曼滤波算法的基础上，提出了对非线性随机动态系统进行学习建模的迭代算法，用这种方法对非线性随机系统建模，可以获得更准确伯系统模型，并可对非线性随机系统进行状态估计。最后给出相应算法及仿真结果。     

非线性系统的可控正则型和状态变换的求法

Zeitz引入了非线性控制系统的可控正则型,证明了由可控正则型描述的非线性系统是可控的,本文进一步给出了非线性系统正则化的条件和状态变换的算法,从而解决了通过状态变换证明非线性系统的可控性。     

Testing the no-hair theorem with observations of black holes in the electromagnetic spectrum

According to the no-hair theorem, astrophysical black holes are uniquely described by their mass and spin. In this paper, we review a new framework for testing the no-hair hypothesis with observations in the electromagnetic spectrum. The approach is formulated in terms of a Kerr-like spacetime containing a quadrupole moment that is independent of both mass and spin. If the no-hair theorem is correct, then any deviation from the Kerr metric quadrupole has to be zero. We show how upcoming VLBI imaging observations of Sgr A∗ as well as spectroscopic observations of iron lines from accreting black holes with IXO may lead to the first astrophysical test of the no-hair theorem.     

无依托状态加速度计的新型标定方法

为解决加速度计性能参数时变性的问题,提出了无依托状态下加速度计标定方法.在无需借助转台等传统标定设备、无需拆卸惯性元件的条件下,充分利用惯导系统(INS,Inertial Navigation System)自身资源,以静基座初始对准获得的准确姿态信息为前提,利用当地重力g作为标定基准,考虑到误差模型非线性的特点,引入非线性寻优策略辨识零位偏差,将误差模型蜕变为线性后,运用线性最小二乘方法辨识安装误差矩阵和刻度因数误差,从而实现加速度计关键参数标定.数值仿真结果显示:经过标定后加速度计测量误差可减小20倍,说明在无依托状态下具有工程实用价值.      

余度捷联惯导系统连续自动标定技术

以余度捷联惯导系统为研究对象,提出了一种新的连续自动标定技术.从惯导系统误差模型出发,推导了这种连续自动标定技术的原理方程,指出在特殊旋转路径下由系统导航解算输出的速度误差将包含惯性器件误差的相关信息.依据惯性器件误差逐级分离的观点,设计了标定旋转路径.在设计的转台连续旋转轨迹下,利用卡尔曼滤波器可以获得全部常值误差项的精确估计.通过构建余度捷联系统标定仿真平台验证了这种技术的有效性.仿真结果表明,与传统的多位置翻滚标定方法相比,该技术标定精度高,操作简单易行,具有较好的工程应用价值.     

利用AE指数重构磁层相空间—对存在问题的讨论

1引言由于磁层的物理过程受到太阳风到电离层诸多过程的影响并包含了许多空间和时间尺度，因此磁层是个相当复杂的系统．人们希望通过新的非线性科学理论了解这一系统的基本参数．因而许多学者纷纷用目前能较好反映磁层活动的极光电集流指数AE（或AL）及常用的相空间重构方法对磁层进行研究．他们利用不同时间段的AE指数和GP方法I’域SVD法l’］得到的吸引子的关联维在2－4之间，因此，认为磁层是一个具有低维吸引子的动力学系统．然而有人用修正的QP法l’］详细计算了多个时间段AE指数的关联维，发现计算的关联继大小依赖于磁层的活…