本文關(guān)鍵詞： 費(fèi)米平譜射電類星體 逆康普頓散射 外光子場 Seyfert 1星系　出處：《云南師范大學(xué)》2016年碩士論文　論文類型：學(xué)位論文

【摘要】：本文先對活動(dòng)星系核的特性、基本分類、產(chǎn)能機(jī)制及統(tǒng)一模型做了較為全面的綜述,然后再對費(fèi)米耀變體(Blazars)的一個(gè)子類費(fèi)米平譜射電類星體(FSRQs)的外光子場和賽弗特1星系(Seyfert 1)的黑洞質(zhì)量與宇宙學(xué)紅移等問題進(jìn)行的主要研究。第一章,主要介紹了活動(dòng)星系核的一些基本特性,一般分類及各子類相應(yīng)的性質(zhì),活動(dòng)星系核的主要產(chǎn)能機(jī)制和統(tǒng)一模型;費(fèi)米伽瑪空間望遠(yuǎn)鏡。第二章,介紹了費(fèi)米耀變體(Blazars)的性質(zhì)和輻射特性,以及賽弗特1星系的性質(zhì)。第三章,我們對具有高效的吸積率產(chǎn)生強(qiáng)的外光子場的費(fèi)米平譜射電類星體(FSRQs)進(jìn)行研究,得到以下結(jié)論:(1)逆康普頓散射峰值光度和同步輻射峰值光度之比SICLL/與逆康普頓散射峰值頻率和同步輻射峰值頻率之比SIC??/呈現(xiàn)負(fù)相關(guān)性;(2)逆康普頓散射峰值光度與同步輻射峰值光度之間具有較強(qiáng)的相關(guān)性;(3)對于大多數(shù)的費(fèi)米FSRQs天體,逆康普頓散射峰值光度大于同步輻射峰值光度。這些結(jié)果都表明費(fèi)米平譜射電類星體的種子光子除了來源于寬線區(qū)以外,還可能來源于其它的區(qū)域。并且,噴流的運(yùn)動(dòng)與磁場及外光子的能量密度相關(guān)。第四章,我們對窄線Seyfert 1星系和寬線Seyfert 1星系的四個(gè)物理量(紅移、愛丁頓比、黑洞質(zhì)量和熱光度)各自的分布進(jìn)行了研究,并且還討論了紅移和熱光度,紅移和愛丁頓比之間的關(guān)系,得到如下結(jié)論:窄線Seyfert 1星系出現(xiàn)在宇宙演化的早期,并且其紅移、熱光度、愛丁頓比的平均值都比寬線Seyfert 1星系的平均值大,而黑洞質(zhì)量的平均值比寬線Seyfert 1星系的平均值小,隨著演化的發(fā)展,黑洞對周圍物質(zhì)的吸積作用不斷增大,吸積能量不能維持其吸積過程,吸積率就慢慢下降,當(dāng)演化進(jìn)行到一定時(shí),窄線Seyfert 1星系就過渡到了寬線Seyfert 1星系。
[Abstract]:In this paper, the characteristics, basic classification, productivity mechanism and unified model of AGNs are reviewed. Then the outer photon field and Seyfert 1 of a subclass of the Fermi plane radio quasar FSRQs of the Fermiyao variant Blazars) and the Seyfert 1). Of black hole mass and cosmological redshift. Chapter 1. This paper mainly introduces some basic characteristics of AGNs, general classification and corresponding properties of each subclass, main productivity mechanism and unified model of AGNs. The Fermi Gamma Space Telescope. Chapter 2 introduces the properties and radiation properties of the Fermiyao variant Blazars, as well as the properties of the Severt 1 galaxy. Chapter 3. We study the FSRQs of Fermipin-spectrum radio quasars with high accretion rate and strong external photon field. The ratio of the inverse Compton scattering peak luminosity to the synchrotron radiation peak luminosity / the ratio of the inverse Compton scattering peak frequency to the inverse Compton scattering peak frequency and the synchrotron radiation peak frequency is obtained. ? / negative correlation; (2) there is a strong correlation between the peak luminosity of inverse Compton scattering and the peak luminosity of synchrotron radiation; For most Fermi FSRQs objects. The inverse Compton scattering peak luminosity is greater than the synchrotron radiation peak luminosity. These results indicate that the seed photons of Fermiping spectrum radio quasars may come from other regions besides the wide line region. The motion of the jet is related to the magnetic field and the energy density of the outer photon. In Chapter 4th, we study the four physical quantities (redshift, Eddington ratio) of the narrow-line Seyfert _ 1 galaxy and the wide-line Seyfert _ 1 galaxy. The relationship between red shift and thermal luminosity, redshift and thermal luminosity, redshift and Eddington ratio are also discussed. The conclusions are as follows: the narrow-line Seyfert _ 1 galaxy appeared in the early stage of cosmic evolution, and its redshift, thermal luminosity, and Eddington ratio were larger than those of the wide-line Seyfert _ 1 galaxy. The mean mass of black hole is smaller than that of wide-line Seyfert _ 1 galaxy. With the development of evolution, the accretion effect of black hole on the surrounding matter is increasing, and accretion energy can not maintain its accretion process. The accretion rate decreases slowly, and as the evolution reaches a certain point, the narrow-line Seyfert _ 1 galaxy is transitioned to the wide-line Seyfert _ 1 galaxy.
【學(xué)位授予單位】：云南師范大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2016
【分類號】：P158;P152

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