本文關(guān)鍵詞： 活動(dòng)星系核 噴流 吸積盤(pán)　出處：《中國(guó)科學(xué)院大學(xué)(中國(guó)科學(xué)院云南天文臺(tái))》2016年博士論文　論文類(lèi)型：學(xué)位論文

【摘要】：吸積率是限制活動(dòng)星系核(AGN)中心活動(dòng)最基本的物理量之一。對(duì)應(yīng)不同的吸積率(愛(ài)丁頓比),AGN中心會(huì)形成不同的盤(pán)結(jié)構(gòu),因而表現(xiàn)出不同的觀(guān)測(cè)特征。AGN的吸積性質(zhì)不僅關(guān)系到其自身的觀(guān)測(cè)特征,還與噴流的形成、AGN對(duì)寄主星系的反饋等基礎(chǔ)問(wèn)題密切相關(guān)。由于其顯著的噴流活動(dòng),射電噪AGN的研究在A(yíng)GN研究中一直是最活躍的領(lǐng)域之一。在射電噪AGN的各波段輻射中,噴流非熱輻射都占有很大的比重。因此,目前對(duì)射電噪AGN愛(ài)丁頓比的限制存在很大的不確定性,甚至存在一些互相矛盾的結(jié)論。要限制愛(ài)丁頓比,首先需要準(zhǔn)確地測(cè)量AGN中心黑洞的質(zhì)量。我們利用窄帶測(cè)光,觀(guān)測(cè)了兩個(gè)年輕射電源,目的是通過(guò)反響映射方法來(lái)估計(jì)它們的中心黑洞質(zhì)量。這也是第一次對(duì)這類(lèi)源進(jìn)行的反響映射觀(guān)測(cè)。遺憾的是兩個(gè)源都沒(méi)有觀(guān)測(cè)到延時(shí),但是為以后類(lèi)似觀(guān)測(cè)的選源和觀(guān)測(cè)策略制定積累了一定的經(jīng)驗(yàn)。其次,估計(jì)愛(ài)丁頓比還需要吸積過(guò)程的熱光度。我們分別從X射線(xiàn)和光學(xué)兩個(gè)波段對(duì)年輕射電源的熱光度進(jìn)行限制。年輕射電源的X射線(xiàn)輻射可能來(lái)自噴流,也可能來(lái)自吸積過(guò)程。如果用X射線(xiàn)光度來(lái)估計(jì)熱光度,首先要確定是吸積過(guò)程主導(dǎo)了其X射線(xiàn)輻射。我們分析了年輕射電源的射電/X射線(xiàn)相關(guān)和黑洞基本面關(guān)系,發(fā)現(xiàn)這兩個(gè)關(guān)系都與噴流主導(dǎo)X射線(xiàn)輻射的理論預(yù)言差別很大。因此我們得出結(jié)論,確實(shí)是吸積過(guò)程主導(dǎo)了年輕射電源的X射線(xiàn)輻射。利用X射線(xiàn)光度估計(jì)的愛(ài)丁頓比表明,年輕射電源的愛(ài)丁頓比普遍較高,而且高激發(fā)星系(HEG)和低激發(fā)星系(LEG)沒(méi)有明顯的差別。光學(xué)光譜觀(guān)測(cè)的結(jié)果也表明年輕射電源具有較高的愛(ài)丁頓比。而且除了展寬更寬之外,這些源的光譜特征與窄線(xiàn)賽弗特I型星系(NLS1)非常類(lèi)似。因此年輕射電源很可能是NLS1的高黑洞質(zhì)量對(duì)應(yīng)體。由于噴流非熱輻射貢獻(xiàn)了blazar很大比例的光學(xué)和X射線(xiàn)輻射,我們并沒(méi)有直接估計(jì)blazar的吸積率,而是通過(guò)間接的方法來(lái)對(duì)它們的吸積性質(zhì)進(jìn)行限制。首先,我們嘗試確定影響blazar分類(lèi)的根本原因,對(duì)blazar的吸積性質(zhì)進(jìn)行限制。我們發(fā)現(xiàn)blazar的同步峰頻與多普勒因子具有很強(qiáng)的反相關(guān)。而且這種反相關(guān)與黑洞質(zhì)量同時(shí)決定噴流的體洛倫茲因子和同步峰頻的圖像非常一致。另外,我們發(fā)現(xiàn)觀(guān)測(cè)上FSRQ和BL Lac天體的噴流功率差異也是由多普勒因子的不同造成的。同步峰頻與光度的反相關(guān),即blazar sequence,也在考慮聚束效應(yīng)后變得不再相關(guān)。這也就表明外光子場(chǎng)的冷卻效應(yīng)并不是決定同步峰頻的主要原因。綜合以上結(jié)果,我們認(rèn)為黑洞質(zhì)量的不同導(dǎo)致了體洛倫茲因子的差異,最終導(dǎo)致了blazar能譜和噴流功率的不同。也就是說(shuō),吸積率在blazar分類(lèi)中并不起決定作用。另外,我們對(duì)一個(gè)劇烈活動(dòng)FSRQ—3C 454.3的爆發(fā)態(tài)進(jìn)行了密集的多色測(cè)光觀(guān)測(cè)。在爆發(fā)過(guò)程中,光學(xué)和伽馬射線(xiàn)波段的光變之間存在非常好的相關(guān)性,證實(shí)了blazar高能輻射的輕子模型。同時(shí),3C 454.3的光學(xué)色指數(shù)隨光學(xué)星等表現(xiàn)出越亮越紅的趨勢(shì),表明吸積盤(pán)的輻射確實(shí)在其光學(xué)輻射中占有很大的比重。
[Abstract]:The accretion rate is limited in active galactic nuclei (AGN) is one of the most basic physical activity center. Corresponding to different accretion rates (Eddington), AGN center will form a different disk structure, so that the observed characteristics of.AGN different accretion properties not only related to the observation of its own characteristic, also formed with the jet. Feedback based on AGN host galaxies are closely related. Because of its remarkable jet research activities, radio-loud AGN has been one of the most active fields in the research of AGN. In the AGN band radio noise radiation, non thermal radiation jet has a large proportion. Therefore, the radio noise AGN Eddington than the limitations of great uncertainty, and even the existence of some conflicting conclusions. To limit the Eddington ratio, first need to accurately measure the quality of the hole in the center of AGN. We use narrowband photometry, two young shoots were observed The power, purpose is to estimate their quality through the hole in the center of echo reverberation mapping mapping method. This is also the first observation of this kind of source. Unfortunately the two sources are not observed in delay, but the development of accumulated some experience for the selection of source and observation strategies after similar observations. Secondly, estimation Eddington also need accretion process. We performed the bolometric luminosity limit from X rays and two degrees of thermo optical band young radio sources. X ray radiation young radio sources may come from the jet, may also come from the accretion process. If using X ray luminosity to estimate the bolometric luminosity, first to determine the accretion process leading the X ray radiation. We analyzed the /X ray and radio related black hole fundamental relations between young radio sources, it was found that the two relations with the jet dominant X ray radiation theory predicted the difference. So We conclude that is indeed the accretion process dominated the X radiation source. The young Eddington X is estimated by using the ray luminosity ratio suggests that young radio sources generally higher than Eddington, and highly excited galaxies (HEG) and low excited galaxies (LEG). Results there was no significant difference between the optical spectral observations also next year the light source has a high Eddington ratio. In addition to spread wider, spectral characteristics of these sources and narrow line Seyfert Galaxy I (NLS1) are very similar. So the young radio sources are likely to be high quality black hole counterpart NLS1. Due to the non thermal radiation jet contributed a large proportion of Blazar and X optical radiation, we do not directly estimate the Blazar accretion rate, but by the indirect method of accretion of their properties were limited. First, we try to determine the root cause of the Blazar classification, Blazar To limit the accretion properties. We found that the peak frequency of synchronous Blazar and Doppler factor has a strong anti correlation. And the anti quality and black hole while the decision is very consistent image Lorenz factor jet and synchronous peak frequency. In addition, we found that the observation on FSRQ and BL Lac objects and the jet power difference is also the Doppler factor the difference. The peak frequency and synchronous photometric reverse Blazar, sequence, is also considering the bunching effect and become no longer relevant. This also indicates that the main reason of the photon field cooling effect is not synchronous peak frequency. Based on the above results, we believe that the black hole mass resulted in different body Lorenz the factor, eventually led to the Blazar spectrum and the jet power is different. That is to say, the accretion rate does not play a decisive role in the classification of Blazar. In addition, we on a violent activity FSRQ 454.3 - 3C outbreak of the state of multicolor photometric observations intensive. During the outbreak, there is a good correlation between the optical and gamma ray light, Blazar confirmed the lepton model of high-energy radiation. At the same time, the 3C 454.3 optical color index with optical magnitude showed more bright red trend shows the radiation of the accretion disc is in a large proportion of the optical radiation.

【學(xué)位授予單位】：中國(guó)科學(xué)院大學(xué)(中國(guó)科學(xué)院云南天文臺(tái))
【學(xué)位級(jí)別】：博士
【學(xué)位授予年份】：2016
【分類(lèi)號(hào)】：P145.8;P157.6

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相關(guān)期刊論文 前2條

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本文編號(hào)：1502388