活动星系核中的温吸收

发布时间：2018-04-29 16:34

  本文选题：活动 + 星系　； 参考：《南京大学》2011年博士论文

【摘要】：在对活动星系核的X射线研究之中,温吸收占着很重要的一部分。它所描述的被电离的外流气体,在各个层面上限制着活动星系核的标准模型及其对周围环境的影响。随着观测手段的进步,温吸收展现了前所未有的丰富细节。本论文旨在研究温吸收在不同类型活动星系核中的异同,以及在X射线和紫外波段的相互关联,由此来揭示温吸收的本质。论文的具体结构如下： 第一章是对活动星系核的概述,介绍了标准模型的各个部分作为温吸收起源的可能性。主要包括了尘埃环热驱动所产生的热风,吸积盘的盘风,宽线区和窄线区的云块。同时为了证明活动星系核对周围环境的巨大影响,我们还简单提及了星系团的冷却流,MBH-σ关系和X射线背景。 第二章则重点论述温吸收的物理过程。介绍如何通过原子过程去使气体达到电离平衡与热平衡,以及随时间演化的非平衡电离的重要性。XSTAR软件是这章的另一主要内容,描述如何通过一些具体的物理参数来求得温吸收模型。 第三章总结了从第一次发现温吸收到高分辨率望远镜上天之前这段时间的研究成果。同时描述了高分辨率望远镜：Chandra与XMM-Newton的构造和观测能力。 第四章主要介绍Ⅰ型活动星系核中的温吸收。我们研究了Mrk 290这个典型Ⅰ型活动星系核的Chandra和XMM-Newton光谱数据,并从中发现了3个温吸收组分。这三个温吸收组分共同存在于尘埃环的热风区域,以每年约450kms-1的速度外流,并且在3年的时间里吸收柱密度有了缓慢的增加。这一章还描述了近十年中,一些经典源带来的有趣的结果,以及两个样本分析。 第五章主要介绍Ⅱ型与窄线Ⅰ型活动星系核中的温吸收。我们第一次描述了一个Ⅱ型活动星系核IRAS18325-5926中的温吸收特征。宽窄两个温吸收组分的柱密度在快速变化着,说明它们有很快的横向移动速度。我们建议这两个组分产生于之前高度电离盘的盘风,并且相互连接。这与Ⅰ型活动星系核中的吸积盘风模型相互吻合。窄线Ⅰ型活动星系核的特别的吸积过程,使得其中的温吸收气体也相对复杂。这里主要记录了十年来人们对NGC 4151和NGC 4051这两个源不休的争论与探讨,温吸收的激波模型也在这里被提出来。 第六章研究紫外吸收与温吸收的联系。首先概述了紫外吸收的观测历史与发展。然后介绍了一些紫外吸收与温吸收结合之后带来的新的视角。最后我们研究了Mrk 290的FUSE与HST/COS的光谱,确定了它的紫外吸收与X射线温吸收为同一气体产生。同时我们也探讨了宽线区和窄线区云块的电离水平和产生温吸收的能力。 第七章是对温吸收的简单总结和对将来工作的规划,以及对未来的X射线卫星的展望。
[Abstract]:Temperature absorption is an important part of X-ray studies of active galactic nuclei. The ionized outflow gas described in this paper limits the standard model of active galactic nuclei and its impact on the surrounding environment at all levels. With the development of observation methods, the temperature absorption shows unprecedented rich details. This paper aims to reveal the nature of temperature absorption by studying the similarities and differences of temperature absorption in different types of active galactic nuclei and the correlation between X-ray and ultraviolet bands. The structure of the paper is as follows: The first chapter is an overview of the active galactic nuclei (AGNs) and introduces the possibility of each part of the standard model as the origin of temperature absorption. It mainly includes hot wind generated by heat drive of dust ring, disk wind of accretion disk, cloud block of wide line and narrow line. At the same time, in order to prove the great influence of the active galactic nuclei on the surrounding environment, we also briefly refer to the MBH- 蟽 relation of the cooling flow and the X-ray background of the cluster. The second chapter focuses on the physical process of temperature absorption. This paper introduces how to achieve ionization equilibrium and thermal equilibrium of gas through atomic process, and the importance of nonequilibrium ionization over time. The XSTAR software is another main content of this chapter. This paper describes how to obtain the temperature absorption model by some specific physical parameters. The third chapter summarizes the research results from the first discovery of temperature absorption to the high resolution telescope. The structure and observational capabilities of the high resolution telescopes: Chandra and XMM-Newton are also described. Chapter 4 mainly introduces the temperature absorption in type I active galactic nuclei. We have studied the Chandra and XMM-Newton spectra of Mrk 290, a typical type I active galactic nucleus, from which three temperature absorption components have been found. These three absorption components co-exist in the hot wind region of the dust ring and flow out at an annual rate of about 450kms-1, and the density of the absorption column increases slowly over a period of 3 years. This chapter also describes some interesting results from classical sources and two sample analyses in the last decade. Chapter 5 mainly introduces the temperature absorption in type 鈪，

本文编号：1820717