本文選題：活動 + 星系　； 參考：《南京大學(xué)》2011年博士論文

【摘要】：在對活動星系核的X射線研究之中,溫吸收占著很重要的一部分。它所描述的被電離的外流氣體,在各個(gè)層面上限制著活動星系核的標(biāo)準(zhǔn)模型及其對周圍環(huán)境的影響。隨著觀測手段的進(jìn)步,溫吸收展現(xiàn)了前所未有的豐富細(xì)節(jié)。本論文旨在研究溫吸收在不同類型活動星系核中的異同,以及在X射線和紫外波段的相互關(guān)聯(lián),由此來揭示溫吸收的本質(zhì)。論文的具體結(jié)構(gòu)如下： 第一章是對活動星系核的概述,介紹了標(biāo)準(zhǔn)模型的各個(gè)部分作為溫吸收起源的可能性。主要包括了塵埃環(huán)熱驅(qū)動所產(chǎn)生的熱風(fēng),吸積盤的盤風(fēng),寬線區(qū)和窄線區(qū)的云塊。同時(shí)為了證明活動星系核對周圍環(huán)境的巨大影響,我們還簡單提及了星系團(tuán)的冷卻流,MBH-σ關(guān)系和X射線背景。 第二章則重點(diǎn)論述溫吸收的物理過程。介紹如何通過原子過程去使氣體達(dá)到電離平衡與熱平衡,以及隨時(shí)間演化的非平衡電離的重要性。XSTAR軟件是這章的另一主要內(nèi)容,描述如何通過一些具體的物理參數(shù)來求得溫吸收模型。 第三章總結(jié)了從第一次發(fā)現(xiàn)溫吸收到高分辨率望遠(yuǎn)鏡上天之前這段時(shí)間的研究成果。同時(shí)描述了高分辨率望遠(yuǎn)鏡：Chandra與XMM-Newton的構(gòu)造和觀測能力。 第四章主要介紹Ⅰ型活動星系核中的溫吸收。我們研究了Mrk 290這個(gè)典型Ⅰ型活動星系核的Chandra和XMM-Newton光譜數(shù)據(jù),并從中發(fā)現(xiàn)了3個(gè)溫吸收組分。這三個(gè)溫吸收組分共同存在于塵埃環(huán)的熱風(fēng)區(qū)域,以每年約450kms-1的速度外流,并且在3年的時(shí)間里吸收柱密度有了緩慢的增加。這一章還描述了近十年中,一些經(jīng)典源帶來的有趣的結(jié)果,以及兩個(gè)樣本分析。 第五章主要介紹Ⅱ型與窄線Ⅰ型活動星系核中的溫吸收。我們第一次描述了一個(gè)Ⅱ型活動星系核IRAS18325-5926中的溫吸收特征。寬窄兩個(gè)溫吸收組分的柱密度在快速變化著,說明它們有很快的橫向移動速度。我們建議這兩個(gè)組分產(chǎn)生于之前高度電離盤的盤風(fēng),并且相互連接。這與Ⅰ型活動星系核中的吸積盤風(fēng)模型相互吻合。窄線Ⅰ型活動星系核的特別的吸積過程,使得其中的溫吸收氣體也相對復(fù)雜。這里主要記錄了十年來人們對NGC 4151和NGC 4051這兩個(gè)源不休的爭論與探討,溫吸收的激波模型也在這里被提出來。 第六章研究紫外吸收與溫吸收的聯(lián)系。首先概述了紫外吸收的觀測歷史與發(fā)展。然后介紹了一些紫外吸收與溫吸收結(jié)合之后帶來的新的視角。最后我們研究了Mrk 290的FUSE與HST/COS的光譜,確定了它的紫外吸收與X射線溫吸收為同一氣體產(chǎn)生。同時(shí)我們也探討了寬線區(qū)和窄線區(qū)云塊的電離水平和產(chǎn)生溫吸收的能力。 第七章是對溫吸收的簡單總結(jié)和對將來工作的規(guī)劃,以及對未來的X射線衛(wèi)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，

本文編號：1820717