本文關(guān)鍵詞： 活動星系核 噴流 吸積盤　出處：《中國科學(xué)院大學(xué)(中國科學(xué)院云南天文臺)》2016年博士論文　論文類型：學(xué)位論文

【摘要】：吸積率是限制活動星系核(AGN)中心活動最基本的物理量之一。對應(yīng)不同的吸積率(愛丁頓比),AGN中心會形成不同的盤結(jié)構(gòu),因而表現(xiàn)出不同的觀測特征。AGN的吸積性質(zhì)不僅關(guān)系到其自身的觀測特征,還與噴流的形成、AGN對寄主星系的反饋等基礎(chǔ)問題密切相關(guān)。由于其顯著的噴流活動,射電噪AGN的研究在AGN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,目前對射電噪AGN愛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。要限制愛丁頓比,首先需要準確地測量AGN中心黑洞的質(zhì)量。我們利用窄帶測光,觀測了兩個年輕射電源,目的是通過反響映射方法來估計它們的中心黑洞質(zhì)量。這也是第一次對這類源進行的反響映射觀測。遺憾的是兩個源都沒有觀測到延時,但是為以后類似觀測的選源和觀測策略制定積累了一定的經(jīng)驗。其次,估計愛丁頓比還需要吸積過程的熱光度。我們分別從X射線和光學(xué)兩個波段對年輕射電源的熱光度進行限制。年輕射電源的X射線輻射可能來自噴流,也可能來自吸積過程。如果用X射線光度來估計熱光度,首先要確定是吸積過程主導(dǎo)了其X射線輻射。我們分析了年輕射電源的射電/X射線相關(guān)和黑洞基本面關(guān)系,發(fā)現(xiàn)這兩個關(guān)系都與噴流主導(dǎo)X射線輻射的理論預(yù)言差別很大。因此我們得出結(jié)論,確實是吸積過程主導(dǎo)了年輕射電源的X射線輻射。利用X射線光度估計的愛丁頓比表明,年輕射電源的愛丁頓比普遍較高,而且高激發(fā)星系(HEG)和低激發(fā)星系(LEG)沒有明顯的差別。光學(xué)光譜觀測的結(jié)果也表明年輕射電源具有較高的愛丁頓比。而且除了展寬更寬之外,這些源的光譜特征與窄線賽弗特I型星系(NLS1)非常類似。因此年輕射電源很可能是NLS1的高黑洞質(zhì)量對應(yīng)體。由于噴流非熱輻射貢獻了blazar很大比例的光學(xué)和X射線輻射,我們并沒有直接估計blazar的吸積率,而是通過間接的方法來對它們的吸積性質(zhì)進行限制。首先,我們嘗試確定影響blazar分類的根本原因,對blazar的吸積性質(zhì)進行限制。我們發(fā)現(xiàn)blazar的同步峰頻與多普勒因子具有很強的反相關(guān)。而且這種反相關(guān)與黑洞質(zhì)量同時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)觀測上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,吸積率在blazar分類中并不起決定作用。另外,我們對一個劇烈活動FSRQ—3C 454.3的爆發(fā)態(tài)進行了密集的多色測光觀測。在爆發(fā)過程中,光學(xué)和伽馬射線波段的光變之間存在非常好的相關(guān)性,證實了blazar高能輻射的輕子模型。同時,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,表明吸積盤的輻射確實在其光學(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】：中國科學(xué)院大學(xué)(中國科學(xué)院云南天文臺)
【學(xué)位級別】：博士
【學(xué)位授予年份】：2016
【分類號】：P145.8;P157.6

【參考文獻】

相關(guān)期刊論文 前2條

1 Xu-Liang Fan;Jin-Ming Bai;Ji-Rong Mao;;What determines the observational differences of blazars?[J];Research in Astronomy and Astrophysics;2016年11期

2 張居甲;范玉峰;常亮;王傳軍;易衛(wèi)敏;;云南暗弱天體光譜及成像儀長縫光譜研究[J];天文研究與技術(shù);2012年04期

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本文編號：1502388