射电噪活动星系核的吸积性质研究

发布时间：2018-02-11 06:16

本文关键词： 活动星系核喷流吸积盘　出处：《中国科学院大学(中国科学院云南天文台)》2016年博士论文　论文类型：学位论文

【摘要】：吸积率是限制活动星系核(AGN)中心活动最基本的物理量之一。对应不同的吸积率(爱丁顿比),AGN中心会形成不同的盘结构,因而表现出不同的观测特征。AGN的吸积性质不仅关系到其自身的观测特征,还与喷流的形成、AGN对寄主星系的反馈等基础问题密切相关。由于其显著的喷流活动,射电噪AGN的研究在AGN研究中一直是最活跃的领域之一。在射电噪AGN的各波段辐射中,喷流非热辐射都占有很大的比重。因此,目前对射电噪AGN爱丁顿比的限制存在很大的不确定性,甚至存在一些互相矛盾的结论。要限制爱丁顿比,首先需要准确地测量AGN中心黑洞的质量。我们利用窄带测光,观测了两个年轻射电源,目的是通过反响映射方法来估计它们的中心黑洞质量。这也是第一次对这类源进行的反响映射观测。遗憾的是两个源都没有观测到延时,但是为以后类似观测的选源和观测策略制定积累了一定的经验。其次,估计爱丁顿比还需要吸积过程的热光度。我们分别从X射线和光学两个波段对年轻射电源的热光度进行限制。年轻射电源的X射线辐射可能来自喷流,也可能来自吸积过程。如果用X射线光度来估计热光度,首先要确定是吸积过程主导了其X射线辐射。我们分析了年轻射电源的射电/X射线相关和黑洞基本面关系,发现这两个关系都与喷流主导X射线辐射的理论预言差别很大。因此我们得出结论,确实是吸积过程主导了年轻射电源的X射线辐射。利用X射线光度估计的爱丁顿比表明,年轻射电源的爱丁顿比普遍较高,而且高激发星系(HEG)和低激发星系(LEG)没有明显的差别。光学光谱观测的结果也表明年轻射电源具有较高的爱丁顿比。而且除了展宽更宽之外,这些源的光谱特征与窄线赛弗特I型星系(NLS1)非常类似。因此年轻射电源很可能是NLS1的高黑洞质量对应体。由于喷流非热辐射贡献了blazar很大比例的光学和X射线辐射,我们并没有直接估计blazar的吸积率,而是通过间接的方法来对它们的吸积性质进行限制。首先,我们尝试确定影响blazar分类的根本原因,对blazar的吸积性质进行限制。我们发现blazar的同步峰频与多普勒因子具有很强的反相关。而且这种反相关与黑洞质量同时决定喷流的体洛伦兹因子和同步峰频的图像非常一致。另外,我们发现观测上FSRQ和BL Lac天体的喷流功率差异也是由多普勒因子的不同造成的。同步峰频与光度的反相关,即blazar sequence,也在考虑聚束效应后变得不再相关。这也就表明外光子场的冷却效应并不是决定同步峰频的主要原因。综合以上结果,我们认为黑洞质量的不同导致了体洛伦兹因子的差异,最终导致了blazar能谱和喷流功率的不同。也就是说,吸积率在blazar分类中并不起决定作用。另外,我们对一个剧烈活动FSRQ—3C 454.3的爆发态进行了密集的多色测光观测。在爆发过程中,光学和伽马射线波段的光变之间存在非常好的相关性,证实了blazar高能辐射的轻子模型。同时,3C 454.3的光学色指数随光学星等表现出越亮越红的趋势,表明吸积盘的辐射确实在其光学辐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.

【学位授予单位】：中国科学院大学(中国科学院云南天文台)
【学位级别】：博士
【学位授予年份】：2016
【分类号】：P145.8;P157.6

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