本文選題：活動星系核 + 黑洞質(zhì)量��； 參考：《云南師范大學(xué)》2013年碩士論文

【摘要】：本文主要對活動星系核(AGN)的超大黑洞質(zhì)量、多波段輻射特性、射電噪類星體(RLQs)和射電寧靜類星體(RQQs)之間的關(guān)系、窄線Seyfert1星系(NLS1s)和寬線Seyfert1星系(BLS1s)之間的關(guān)系、高能伽馬射線的輻射機(jī)制、噴流和吸積盤之間的關(guān)系、演化等問題進(jìn)行了一系列的研究。 第一章，簡單介紹了活動星系核的基本概念、分類、模型；目前活動星系核黑洞質(zhì)量的主要估算方法；多波段輻射特性；Fermi伽馬空間望遠(yuǎn)鏡；甚高能伽馬射線；AGN伽馬射線輻射機(jī)制。 第二章，收集了117個(gè)類星體(97個(gè)射電噪類星體(RLQs)和20個(gè)射電寧靜類星體(RQQs))的熱光度、H發(fā)射線寬度、射電光學(xué)強(qiáng)度比R、5100的單色光度、紅移，并且計(jì)算了黑洞質(zhì)量、愛丁頓比、總的5GHz射電光度。得到如下結(jié)論：(1)RLQs的黑洞質(zhì)量和射電光學(xué)強(qiáng)度比R、射電光度、熱光度之間具有強(qiáng)的相關(guān)性，而RQQs的黑洞質(zhì)量和射電光學(xué)強(qiáng)度比R、射電光度、熱光度之間具有弱的相關(guān)性；(2)RLQs的射電光度、熱光度、5100的單色光度之間具有強(qiáng)的相關(guān)性，而RQQs的射電光度、熱光度、5100的單色光度之間具有弱的相關(guān)性；(3)RLQs和RQQs的黑洞質(zhì)量、發(fā)射線寬度、愛丁頓比不同；從這些結(jié)果中可以得到：RLQs和RQQs黑洞質(zhì)量的不同可能是由于它們發(fā)射線寬度不同造成的；RLQs和RQQs本質(zhì)不同很可能是它們內(nèi)秉物理性質(zhì)不同引起的；黑洞質(zhì)量、愛丁頓比、寄主星系的形態(tài)、黑洞自旋是解釋雙峰狀分布和射電光學(xué)強(qiáng)度比R的重要參量；射電噴流和吸積盤之間具有緊密的聯(lián)系。 第三章，收集了142個(gè)類星體(114個(gè)射電噪類星體和28個(gè)射電寧靜類星體)，82個(gè)瓣占優(yōu)型射電類星體(LDQ)和43個(gè)核占優(yōu)型射電類星體(CDQ)，80個(gè)Seyfert星系的樣本，基于Logistic非線性回歸分析的方法對紅移和黑洞質(zhì)量、熱光度、5GHz射電光度、愛丁頓比、核主導(dǎo)參數(shù)的關(guān)系進(jìn)行研究。擬合出相應(yīng)的演化曲線。得到如下結(jié)論：(1)類星體的演化是從射電噪類星體到射電寧靜類星體，當(dāng)演化到一定階段類星體過渡到Seyfert星系；(2)瓣占優(yōu)型類星體(LDQ)和核占優(yōu)型類星體(CDQ)之間并沒有明顯地隨紅移演化。 第四章，從斯隆數(shù)字巡天(SDSS)中收集了214個(gè)Seyfert1星系包括147個(gè)窄線Seyfert1星系(NLS1s)和67個(gè)寬線Seyfert1星系(BLS1s)。對兩類Seyfert1星系的黑洞質(zhì)量、核球速度彌散度、愛丁頓比、紅移、5100光度進(jìn)行了研究。得到：(1)在進(jìn)行黑洞質(zhì)量估算時(shí)，應(yīng)該考慮輻射壓的影響，特別是對于窄線Seyfert1星系(NLS1s)；(2)當(dāng)考慮輻射壓時(shí)，窄線Seyfert1星系(NLS1s)的吸積未超愛丁頓吸積，并且滿足了近距正常星系的M BH關(guān)系；(3)驗(yàn)證了從窄線Seyfert1星系(NLS1s)到寬線Seyfert1星系(BLS1s)的演化。 第五章，通過對TeV活動星系核Fermi伽馬射線和多波段輻射的研究，我們得到：(1)對于TeV HSP BL Lacs(THBLs)，在所有的態(tài)(高態(tài)、平均態(tài)、低態(tài))下，F(xiàn)和FR之間，F(xiàn)和FI R之間具有強(qiáng)的相關(guān)性；(2)TeV射電星系(TRGs)偏離了THBLs所占的區(qū)域；(3)和THBLs相比，TeV平譜射電類星體(TFSRQs)有更強(qiáng)的γ射線輻射；(4)對于THBLs，在所有態(tài)下，F(xiàn)和FX之間有弱的相關(guān)性，，并且在高態(tài)和平均態(tài)，F(xiàn)和FO有弱的相關(guān)性，在低態(tài)下F和FO有強(qiáng)的相關(guān)性；(5)對于THBLs，低態(tài)和高態(tài)的FO和FR之間，所有態(tài)的FO和FI R之間，所以態(tài)的FIR和FR之間存在強(qiáng)的相關(guān)性，其它波段之間沒有發(fā)現(xiàn)強(qiáng)的相關(guān)性；(6)對于THBLs，同步自康普頓(SSC)是主要的高能γ射線輻射機(jī)制，并且逆康普頓(IC)散射核周圍的塵埃很可能是個(gè)重要的補(bǔ)充機(jī)制；(7)和THBLs相比，TRGs和TFSRQs可能有不同的高能γ射線起源。 第六章，通過對Fermi平譜射電類星體(FSRQs)寬發(fā)射線光度和多波段光度的研究。我們得到：對于FSRQs，log L和log LBLR之間，log LX和log LBLR之間，log LO和log LBLR之間，log LR和log LBLR之間有顯著的相關(guān)性；log LIR和log LBLR之間的相關(guān)性不顯著(P0.08)，但可以認(rèn)為有顯著相關(guān)的“趨勢”。這些結(jié)果支持了噴流的形成和吸積盤之間有緊密的聯(lián)系。并且log L和log LBLR之間的顯著相關(guān)暗示了FSRQs的伽馬射線的輻射機(jī)制是逆康普頓散射來自寬線區(qū)(BLR)或外流BLR的種子光子。
[Abstract]:In this paper , the relationship between large black hole mass , multi - band radiation characteristic , radio - noise quasar ( RLQs ) and radio quiet quasar ( RQQs ) of active galactic nuclei ( AGN ) is studied .

In chapter one , the basic concept , classification and model of active galactic nuclei are briefly introduced .
The main methods of estimating the quality of the nuclear black holes in active galaxies are presented .
Multi - band radiation characteristics ;
Fermi - gamma space telescope
very high energy gamma rays ;
AGN Gamma Ray Radiation Mechanism .

In chapter 2 , 117 quasars ( 97 radio noise quasars ( RLQs ) and 20 radio silent quasars ( RQQs ) are collected , the widths of H emission lines , the ratio of the radio intensity to the monochromatic light of R and 5100 , the red shift are calculated , and the black hole quality , the Edinburgh ratio and the total 5 GHz radio luminosity are calculated . The following conclusions are obtained : ( 1 ) The black hole quality and the radio optical intensity ratio R , the radio luminosity and the thermal luminosity of the RLQs have strong correlation , while the black hole quality and the radio optical intensity ratio R , the radio luminosity and the thermal luminosity of the RQQs have weak correlation ;
( 2 ) there is a strong correlation between the radio luminosity , the thermal luminosity and the monochromatic light intensity of the RLQs , while the RQQs have a weak correlation between the radio luminosity , the thermal luminosity and the monochromatic light intensity of 5100 .
( 3 ) The quality of black holes , the width of the emission lines and the ratio of Edinburgh to RLQs and RQQs are different ;
From these results , it can be found that the differences in the quality of RLQs and RQQs black holes may be due to the different widths of their transmission lines ;
RLQs and RQQs are different in nature and may be caused by different intrinsic physical properties ;
The black hole mass , the Edinburgh ratio , the shape of the host galaxy , the spin of the black hole are important parameters for explaining the bimodal distribution and the radio - optical intensity ratio R ;
there is a close relationship between the radio jet and the accretion disk .

In chapter 3 , we collected 142 quasars ( 114 radio noise quasars and 28 radio silent quasars ) , 82 lobes dominant radio - quasars ( LDQ ) and 43 nuclear - dominant radio - quasars ( CDQ ) , and investigated the relationship between red shift and black hole mass , thermal luminosity , 5 GHz radio luminosity , Edinburgh ratio and nuclear dominant parameters based on Logistic non - linear regression analysis .
( 2 ) There is no obvious evolution of the red shift between the lobe - dominated quasar ( LDQ ) and the nuclear - dominated quasar ( CDQ ) .

In chapter 4 , we collected 214 galaxies from the Slong Digital Tour ( SDSS ) , including 147 narrow lines ( NLS1s ) and 67 broad - lines ( BLS1s ) galaxies . We studied the black hole quality , the velocity dispersion of the nuclear sphere , the ratio of Edinburgh , red shift , 5100 luminosity to the two types of galaxies .
( 2 ) When considering the radiation pressure , the accretion of the narrow - line Sefert1 galaxy ( NLS1s ) is not super - Edinburgh accretion , and the M - BH relation of the close - range normal galaxy is satisfied ;
( 3 ) The evolution of the galaxy ( NLS1s ) from the narrow line to the wide line of galaxies ( BLS1s ) is verified .

In the fifth chapter , we obtain : ( 1 ) For TeV HSP BL Lacs , we obtain : ( 1 ) There is strong correlation between F and FR between F and FR in all states ( high , average and low states ) for TeV HSP BL Lacs ( THallop ) .
( 2 ) The TeV radio galaxy ( TRGs ) deviates from the region occupied by THECK ;
( 3 ) The TeV flat - spectrum radio - quasar ( TFSRQs ) has stronger 緯 - ray radiation than that of THB .
( 4 ) In all states , there is a weak correlation between F and FX in all states , and F and FO are strongly correlated in high and average states , and F and FO are strongly correlated in low states ;
( 5 ) There is strong correlation between the FO and FRs of all states , and there is strong correlation between the states ' FIR and FR , and there is no strong correlation between the other bands .
( 6 ) The synchronous self - compton ( SSC ) is the main high - energy 緯 - ray radiation mechanism , and the dust around the scattering core of the inverse compton ( IC ) is probably an important supplementary mechanism .
( 7 ) TRGs and TFSRQs may have different origins of high - energy 緯 - ray compared with THEC2 .

In chapter 6 , we obtain the correlation between log L and log LBLR , log LO and log LBLR , log LR and log LBLR between log LX and log LBLR for FSRQs , log L and log LBLR .
The correlation between log LIR and log LBLR is not significant ( P0 . 08 ) , but it may be considered a significant correlation " trend " . These results support a close link between the formation of the jet and the accretion disk , and the significant correlation between log L and log LBLR implies that the radiation mechanism of the gamma rays of the FSRQs is the seed photons scattered from the wide line region ( BLR ) or the outer stream BLR .

【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】：2013
【分類號】：P145.8

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