【摘要】：活動(dòng)星系核是一類中央核區(qū)活動(dòng)性很強(qiáng)的河外星系。這些星系顯得比正常星系活躍，可以輻射出從射電到γ射線的全波段的電磁波。自上世紀(jì)60年代類星體被發(fā)現(xiàn)以來，又相繼發(fā)現(xiàn)了許多具有類似特征的天體，都是河外星系，統(tǒng)稱為活動(dòng)星系核。 根據(jù)標(biāo)準(zhǔn)模型，黑洞-吸積盤模型，目前普遍認(rèn)為類星體是由位于星系中心位置的超大質(zhì)量黑洞和吸積盤構(gòu)成。此外，還引入了寬線區(qū)和窄線區(qū)，以便解釋發(fā)射線光譜。黑洞質(zhì)量的大小對(duì)于幫助我們了解宇宙的早期以及超大質(zhì)量黑洞的形成和演化有著重要的作用，也是類星體研究工作的一個(gè)基本問題。本文就是利用寬發(fā)射線的光度和譜線寬度來估算類星體中心黑洞質(zhì)量，并把估算的結(jié)果與其他方法估算出的結(jié)果相比較，，看是否跟之前吳學(xué)兵等人提出的觀點(diǎn)相吻合。 第一章介紹活動(dòng)星系核的觀測(cè)特征和分類，類星體的概述和發(fā)射線、類星體的黑洞-吸積盤模型。 第二章介紹了類星體中心黑洞質(zhì)量的估算方法的來源以及改進(jìn)和發(fā)展，然后針對(duì)吳學(xué)兵等人提出的連續(xù)譜的光度有可能被觀測(cè)方向上的噴流污染，從而影響了黑洞質(zhì)量的估算結(jié)果，造成偏大效果的觀點(diǎn)，我們構(gòu)建了一個(gè)基于RASS-SDSS-FIRST-GB6交叉認(rèn)證過的射電陡譜源樣本，此樣本中包含了185個(gè)源。這些源的性質(zhì)目錄數(shù)據(jù)中已經(jīng)給出了Shen等人利用連續(xù)譜估算得到的維里黑洞質(zhì)量。我們利用數(shù)據(jù)中給出的這些源的Hβ,MgII,CIV寬發(fā)射線的光度和這些寬發(fā)射線相應(yīng)的FWHM，通過相關(guān)經(jīng)驗(yàn)公式的估算從而得到黑洞質(zhì)量，然后用這些黑洞質(zhì)量跟Shen的維里黑洞質(zhì)量進(jìn)行比較，發(fā)現(xiàn)通過CIV寬發(fā)射線估算得到的黑洞質(zhì)量比維里質(zhì)量要小，對(duì)于樣本里的絕大多數(shù)源都如此，但同樣的情況在通過Hβ,MgII寬發(fā)射線估算的黑洞質(zhì)量跟維里黑洞質(zhì)量的比較中并未出現(xiàn)。 第三章做了一個(gè)簡單的總結(jié)和展望。
[Abstract]:Active galactic nuclei (AGNs) are a class of extragalactic galaxies with strong activity in the central nucleus region. These galaxies appear to be more active than normal galaxies, radiating full-band electromagnetic waves from radio to 緯-rays. Since the discovery of quasars in the 1960s, many objects with similar characteristics have been discovered, all of which are extragalactic, collectively known as active galactic nuclei (AGNs). According to the standard model, black hole accretion disk model, it is generally believed that quasars are composed of supermassive black holes and accretion disks located in the center of galaxies. In addition, broad and narrow line regions are introduced to explain the emission line spectrum. Black hole mass plays an important role in understanding the early universe and the formation and evolution of supermassive black holes. It is also a basic problem in quasar research. In this paper, the mass of a quasar central black hole is estimated by using the luminosity and spectral line width of the broad emission line, and the estimated results are compared with those obtained by other methods to see if it is consistent with the viewpoint put forward by Wu Xuebing et al. The first chapter introduces the observational characteristics and classification of active galactic nuclei, the overview and emission lines of quasars, and the black hole accretion disk model of quasars. In the second chapter, the source, improvement and development of the method for estimating the mass of a quasar central black hole are introduced, and then the luminosity of the continuous spectrum proposed by Wu Xuebing and others may be polluted by a jet in the observed direction. Therefore, we construct a radio steep-spectrum source sample based on RASS-SDSS-FIRST-GB6 cross-authentication, which contains 185 sources. The properties of these sources in the catalog data have been given by Shen et al., using continuous spectra to estimate the mass of the Wirelli black hole. We obtain the mass of black hole by using the luminosity of the H 尾 Mg-III CIV wide emission line given in the data and the FWHM, corresponding to these wide emission lines through the estimation of relevant empirical formulas, and then compare the mass of these black holes with those of Shen's Wirelli black hole. It is found that the mass of black hole estimated by the CIV wide emission line is smaller than that of the Wirelli mass, which is true for most of the sources in the sample. However, the same situation is not found in the comparison between the mass of black hole estimated by H 尾 -MgII wide emission line and the mass of Virie black hole. The third chapter makes a simple summary and prospect.
【學(xué)位授予單位】：廣州大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2012
【分類號(hào)】：P145.8

【參考文獻(xiàn)】

相關(guān)碩士學(xué)位論文 前2條

1 陳志福;SDSS類星體譜線的測(cè)量及其應(yīng)用[D];廣州大學(xué);2011年

2 張春玲;FRIs和FRIIs星系觀測(cè)性質(zhì)的研究[D];廣州大學(xué);2010年

本文編號(hào)：2202550