黑洞系统的大尺度磁场提能机制与准周期振荡
发布时间：2018-09-14 14:20
【摘要】：黑洞等致密天体的辐射通常呈现出快速的变化,有些x射线光变表现出持续稳定的近似周期性,被称为准周期振荡(QPO)。黑洞双星、中等质量黑洞和活动星系核(AGNs)都被观测到存在QPO。由于其时标与黑洞吸积盘内区的动力学时标相当,QPO被认为是探测黑洞附近吸积过程的有效途径。大尺度磁场在高能天体物理中扮演了重要角色,本文在大尺度磁场提能的基础上建立了黑洞双星的3：2高频QPO模型以及不同尺度黑洞系统的QPO统一模型,将QPO频率的产生与辐射谱联系起来。 本轮共振模型自然地解释了3：2高频QPO的小整数比,但是能否克服吸积流的阻尼力对其来说是严重的困难。黑洞与吸积盘之间的磁耦合过程将旋转黑洞的能量和角动量转移到吸积盘内区,克服了共振团块在吸积流中遇到的阻尼力问题,并有利于建立QPO与谱态之间的联系。本文第二章将共振模型和黑洞与吸积盘之间的磁耦合过程结合起来,拟合了三个黑洞双星的3：2高频QPO以及对应的x射线谱形,表明3：2高频QPO是与陡幂律态成协的。 黑洞双星、中等质量黑洞和AGNs在观测上表现出相似性和统一性,本文第三章尝试建立不同尺度黑洞系统的QPO统一模型。Kerr度规下黑洞吸积盘上的环向面电流分布会产生盘盘耦合的闭合大尺度磁场位形,我们考虑了磁耦合过程与盘冕系统的相互作用,利用盘上闭合磁力线的磁重联分别拟合了三种不同尺度黑洞系统的QPO以及对应的x射线谱形。 黑洞双星的谱态转变呈现出纷繁复杂的现象,本文第四章试图用大尺度磁场位形的演化描述态转变,其中涉及到BZ、MC、BP三种大尺度磁场的提能机制。描述盘上磁场集中程度的幂律指数n起着关键作用,随着n的减小,BZ和BP过程的磁场先后消失,黑洞双星由低硬态过渡到硬中间态再转变到陡幂律态。我们拟合了这几个态的主要特征,并估计了由陡幂律态向热主导态转变的时标。描述黑洞双星态转变的HID图中的“喷流线”可以用a*和n参数空间中的临界线得到很好的说明。 吸积盘上的发射线是探测盘内区的另一个有效途径,由于相对论效应,发射线被远处的观测者接收时变得很宽,铁Kα线最为明显。如果将QPO与铁Kα线结合起来,则有可能对吸积盘内区的特性作出更准确的判断。本文第五章利用大尺度磁场的磁耦合过程讨论了黑洞双星的3：2高频QPO与展宽的铁Kα线之间的可能关联。施加在吸积盘内边缘的外部力矩和非轴对称大尺度磁场的螺旋不稳定性分别在盘上产生内外热斑,双热斑的开普勒运动形成3：2 QPO。另一方面,由于内边缘力矩和大尺度磁场MC过程的作用,盘上的辐射很集中,随着半径的增加发射率衰减很快,由该发射率指数计算得到的铁Kα线展宽轮廓与观测值相吻合。
[Abstract]:The radiation of dense celestial bodies such as black holes usually changes rapidly. Some x-ray light changes show a continuous and stable approximate periodicity, which is called quasi-periodic oscillation (QPO). Black hole binaries, medium mass black holes, and active galactic nucleus (AGNs) are all observed to exist QPO. QPO is considered to be an effective way to detect accretion process near a black hole because its time scale is equivalent to the dynamic time scale in the accretion disk of a black hole. Large-scale magnetic field plays an important role in high-energy astrophysics. In this paper, the 3:2 high-frequency QPO model of black hole binaries and the unified QPO model of black hole systems with different scales are established based on the large-scale magnetic field. The generation of QPO frequency is associated with the radiation spectrum. The resonance model naturally explains the small integer ratio of 3:2 high frequency QPO, but it is very difficult to overcome the damping force of accretion flow. The magnetic coupling process between the black hole and the accretion disk transfers the energy and angular momentum of the rotating black hole to the accretion disk, which overcomes the damping force of the resonant mass in the accretion flow and facilitates the establishment of the relationship between the QPO and the spectral states. In the second chapter, by combining the resonance model with the magnetic coupling process between black hole and accretion disk, the 3:2 high frequency QPO and the corresponding X ray spectrum of three black hole binary stars are fitted. It is shown that 3:2 high frequency QPO is associated with the steep power law state. Black hole binaries, medium mass black holes and AGNs show similarity and uniformity in observation. In chapter 3, we try to establish the QPO unified model of black hole systems with different scales. Under the Kerr metric, the toroidal current distribution on the accretion disk of a black hole will produce a disk-coupled closed large-scale magnetic field configuration. The interaction between the magnetic coupling process and the coronal system is considered. The magnetic reconnection of the closed magnetic field line on the disk is used to fit the QPO and the corresponding X ray spectra of three different size black hole systems respectively. The spectral state transition of black hole binary stars presents a complicated phenomenon. In chapter 4, we try to describe the state transition with the evolution of large scale magnetic field configuration, which involves the three kinds of energy raising mechanisms of BZ,MC,BP magnetic field. The power law exponent n, which describes the degree of magnetic field concentration on the disk, plays a key role. With the decrease of n, the magnetic field of the BZ and BP processes disappears successively, and the black hole binary stars transition from the low hard state to the hard intermediate state and then to the steep power law state. We fit the main characteristics of these states and estimate the time scale of the transition from the steep power law state to the thermal dominant state. The "jet line" in the HID diagram describing the transformation of black hole binary states can be well illustrated by the critical lines in a * and n parameter spaces. The emission line on the accretion disk is another effective way to detect the inner region of the disk. Because of the relativistic effect, the emission line becomes very wide when it is received by the remote observer, and the iron K 伪 line is the most obvious. If the QPO is combined with the iron K 伪 line, it is possible to make a more accurate judgment on the characteristics of the accretion disk. In chapter 5, the possible correlation between the 3:2 high frequency QPO of black hole binary stars and the broadened iron K 伪 line is discussed by using the magnetic coupling process of the large scale magnetic field. The external torque applied on the edge of the accretion disk and the helical instability of the non-axisymmetric large-scale magnetic field produced internal and external heat spots on the disk, respectively. The Kepler motion of the double hot spots formed 3:2 QPO.. On the other hand, due to the effect of the internal edge moment and the MC process of the large-scale magnetic field, the radiation on the disk is very concentrated, and the emissivity decays rapidly with the increase of the radius. The broadening profile of the iron K 伪 line calculated from the emissivity exponent is in agreement with the observed values.
【学位授予单位】：华中科技大学
【学位级别】：博士
【学位授予年份】：2011
【分类号】：P145.8
本文编号：2242955
[Abstract]:The radiation of dense celestial bodies such as black holes usually changes rapidly. Some x-ray light changes show a continuous and stable approximate periodicity, which is called quasi-periodic oscillation (QPO). Black hole binaries, medium mass black holes, and active galactic nucleus (AGNs) are all observed to exist QPO. QPO is considered to be an effective way to detect accretion process near a black hole because its time scale is equivalent to the dynamic time scale in the accretion disk of a black hole. Large-scale magnetic field plays an important role in high-energy astrophysics. In this paper, the 3:2 high-frequency QPO model of black hole binaries and the unified QPO model of black hole systems with different scales are established based on the large-scale magnetic field. The generation of QPO frequency is associated with the radiation spectrum. The resonance model naturally explains the small integer ratio of 3:2 high frequency QPO, but it is very difficult to overcome the damping force of accretion flow. The magnetic coupling process between the black hole and the accretion disk transfers the energy and angular momentum of the rotating black hole to the accretion disk, which overcomes the damping force of the resonant mass in the accretion flow and facilitates the establishment of the relationship between the QPO and the spectral states. In the second chapter, by combining the resonance model with the magnetic coupling process between black hole and accretion disk, the 3:2 high frequency QPO and the corresponding X ray spectrum of three black hole binary stars are fitted. It is shown that 3:2 high frequency QPO is associated with the steep power law state. Black hole binaries, medium mass black holes and AGNs show similarity and uniformity in observation. In chapter 3, we try to establish the QPO unified model of black hole systems with different scales. Under the Kerr metric, the toroidal current distribution on the accretion disk of a black hole will produce a disk-coupled closed large-scale magnetic field configuration. The interaction between the magnetic coupling process and the coronal system is considered. The magnetic reconnection of the closed magnetic field line on the disk is used to fit the QPO and the corresponding X ray spectra of three different size black hole systems respectively. The spectral state transition of black hole binary stars presents a complicated phenomenon. In chapter 4, we try to describe the state transition with the evolution of large scale magnetic field configuration, which involves the three kinds of energy raising mechanisms of BZ,MC,BP magnetic field. The power law exponent n, which describes the degree of magnetic field concentration on the disk, plays a key role. With the decrease of n, the magnetic field of the BZ and BP processes disappears successively, and the black hole binary stars transition from the low hard state to the hard intermediate state and then to the steep power law state. We fit the main characteristics of these states and estimate the time scale of the transition from the steep power law state to the thermal dominant state. The "jet line" in the HID diagram describing the transformation of black hole binary states can be well illustrated by the critical lines in a * and n parameter spaces. The emission line on the accretion disk is another effective way to detect the inner region of the disk. Because of the relativistic effect, the emission line becomes very wide when it is received by the remote observer, and the iron K 伪 line is the most obvious. If the QPO is combined with the iron K 伪 line, it is possible to make a more accurate judgment on the characteristics of the accretion disk. In chapter 5, the possible correlation between the 3:2 high frequency QPO of black hole binary stars and the broadened iron K 伪 line is discussed by using the magnetic coupling process of the large scale magnetic field. The external torque applied on the edge of the accretion disk and the helical instability of the non-axisymmetric large-scale magnetic field produced internal and external heat spots on the disk, respectively. The Kepler motion of the double hot spots formed 3:2 QPO.. On the other hand, due to the effect of the internal edge moment and the MC process of the large-scale magnetic field, the radiation on the disk is very concentrated, and the emissivity decays rapidly with the increase of the radius. The broadening profile of the iron K 伪 line calculated from the emissivity exponent is in agreement with the observed values.
【学位授予单位】：华中科技大学
【学位级别】：博士
【学位授予年份】：2011
【分类号】：P145.8
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