本文選題：星系 + 中心��； 參考：《中國(guó)科學(xué)技術(shù)大學(xué)》2014年博士論文

【摘要】：本文主要討論了在冷暗物質(zhì)宇宙中暗物質(zhì)暈等級(jí)成團(tuán)模型下,星系中心的黑洞以暗物質(zhì)暈并合樹為背景的演化和增長(zhǎng)過程。我們根據(jù)前人的工作,在擴(kuò)展的PS(extended Press-Schechter)公式基礎(chǔ)上發(fā)展了一套自己的Monte Carlo算法,建立了暗物質(zhì)暈的并合樹結(jié)構(gòu)。星系中心的種子黑洞是原初星系中的POPⅢ恒星演化后期所形成。隨著暗暈的并合,種子黑洞將會(huì)通過動(dòng)力學(xué)粘滯轉(zhuǎn)移到星系中心去,并帶來一部分氣體。這些黑洞在星系及暗暈的并合后,會(huì)在周圍形成吸積盤,通過吸積盤吸積星系中的氣體,從而質(zhì)量增加。黑洞的活躍過程主要是星系的主并和過程導(dǎo)致的,然后黑洞會(huì)以Eddington吸積率持續(xù)吸積,直到達(dá)到所在星系的M一σ*關(guān)系限定的黑洞質(zhì)量。如果兩個(gè)并合的星系中都有黑洞,會(huì)在星系中心形成雙黑洞系統(tǒng),雙黑洞的演化,最終的并合階段還會(huì)輻射引力波。通過一系列的Monte Carlo模擬,我們能得到AGN(活動(dòng)的黑洞)的光度函數(shù),并和觀測(cè)上的AGN的光度函數(shù)比較。我們用了幾種黑洞吸積盤模型,把Monte Carlo模擬計(jì)算得到的理論值跟觀測(cè)的AGN光度函數(shù)進(jìn)行了比較。除了光度函數(shù),也可以黑洞的質(zhì)量密度。 我們根據(jù)已有的黑洞吸積物理,引入了直接吸積和隨機(jī)吸積兩種黑洞吸積模型在我們的模型中,研究了自旋對(duì)黑洞演化的影響以及大質(zhì)量黑洞并合率的變化。直接吸積盤模型下,光度函數(shù)跟觀測(cè)比偏離比較大。隨機(jī)吸積模型下雖然能比較好的符合光度函數(shù),但是還是有一定的偏離。我們又在直接吸積模型的基礎(chǔ)上,我們考慮了MHD數(shù)值模擬結(jié)果對(duì)吸積盤的影響-黑洞吸積盤的數(shù)值模擬結(jié)果的影響(MHD吸積盤中吸積物質(zhì)對(duì)黑洞自旋及質(zhì)量增長(zhǎng)和理論計(jì)算的不一樣,因?yàn)榇艌?chǎng)關(guān)系有所偏離),并用數(shù)值模擬得出的結(jié)果應(yīng)用到黑洞吸積過程,模擬了星系中心大質(zhì)量黑洞的演化過程,發(fā)現(xiàn)其結(jié)果比單純的直接吸積模型以及隨機(jī)吸積模型都要好,跟光測(cè)上的光度函數(shù)更符合。 有了接近真實(shí)的描述星系中心黑洞演化歷史的模型,我們考慮了不同的雙黑洞演化機(jī)制對(duì)其質(zhì)量比的影響。雙黑洞的演化分為三個(gè)階段：1,各自和周圍恒星的動(dòng)力學(xué)粘滯而落入星系中心；2,動(dòng)力學(xué)粘滯不有效后的三體作用拋恒星過程；3,引力波輻射階段。在雙黑洞演化的第二個(gè)階段,如果存在共轉(zhuǎn)氣體吸積盤,星系中心的雙黑洞質(zhì)量比在雙黑洞演化的前期和后期將會(huì)有明顯的變化,其統(tǒng)計(jì)分布將會(huì)變平。我們拿不同的模擬結(jié)果跟SDSS觀測(cè)到的并合中的星系中的黑洞質(zhì)量比做了比較。發(fā)現(xiàn)模型中主并和條件p0.3的結(jié)果,對(duì)觀測(cè)有較好的符合。在此基礎(chǔ)上加入共轉(zhuǎn)吸積盤的影響,看其質(zhì)量比的統(tǒng)計(jì)分布,發(fā)現(xiàn)在雙黑洞演化的前提,其質(zhì)量比分布會(huì)變平；而在并合后期,其質(zhì)量比分布中有更多的質(zhì)量比接近1的雙黑洞。 在成功的建立了黑洞和暗物質(zhì)暈宇宙學(xué)演化模型后,我們?cè)诖嘶A(chǔ)上,還對(duì)空間引力波探測(cè)器(ALIA)參數(shù)空間的設(shè)定做了一定的討論,爭(zhēng)取能讓空間探測(cè)器能對(duì)高紅移黑洞成長(zhǎng)模型和演化做一定的限制。在ALIA的臂長(zhǎng)比LISA小一個(gè)量級(jí)的情況下,降低對(duì)儀器的要求后,還能讓ALIA對(duì)于中等質(zhì)量的雙黑洞并合率的探測(cè)率比LISA要好不少,為儀器設(shè)計(jì)提供了很好的工具。以后還將進(jìn)行更多的引力波源方面的研究。 模型所用的宇宙學(xué)參數(shù)如下：QM=0.3,ΩA=0.7,h=0.7,Ωbh2=0.02,σ8=0.93和n=1.其中h的定義如下H0=h×100km s-1Mpc-1.
[Abstract]:This paper mainly discusses the process of evolution and growth of black holes in the center of galaxies under the dark matter halo of the dark matter halo in the universe in the cold dark matter universe. Based on the previous work, we developed a set of its own Monte Carlo algorithm based on the extended PS (extended Press-Schechter) formula, and established the dark objects. The seed black hole in the center of the galaxy is formed in the late stage of the evolution of the POP iii star in the original galaxy. With the combination of dark halo, the seed black hole will transfer to the center of the galaxy by kinetic viscosity and bring a part of the gas. The disk accumulates the gas in galaxies and increases the mass of the galaxies. The active process of the black hole is mainly caused by the principal and process of the galaxies, and then the black hole will continue to accret with the Eddington accretion rate until the mass of the black hole defined by the M 1 * relationship of the galaxy. If there are black holes in the two combined galaxies, the double black will be formed at the center of the galaxy. Through a series of Monte Carlo simulations, we can get the photometric function of the AGN (active black hole) and compare with the photometric function of the observed AGN. We use several black hole accretion disk models to simulate the theoretical values obtained by the Monte Carlo simulation and the observed A The luminosity function of GN is compared. Besides the luminosity function, it can also be the mass density of black hole.
Based on the existing black hole accretion physics, we introduce two black hole accretion models of direct accretion and random accretion in our model. We study the influence of spin on the evolution of black hole and the change of the coincidence rate of massive black holes. Under the direct accretion disk model, the luminosity function is much larger than the observation ratio. The ratio of random accretion model is comparable to that of the random accretion model. On the basis of the direct accretion model, we consider the effect of the MHD numerical simulation on the accretion disk - the effect of the numerical simulation of the black hole accretion disk (the accretion substance in the accretion disk of the accretion disk of the MHD accretion disk is different to the black hole spin and the mass growth and the theoretical calculation, " The magnetic field relationship is deviated from the black hole. The numerical simulation results are applied to the black hole accretion process, and the evolution process of the massive black hole in the center of the galaxy is simulated. It is found that the result is better than the simple direct accretion model and the random accretion model, which is more consistent with the photometric function in the light measurement.
With a near real model describing the evolution history of the galaxy's central black hole, we consider the effect of different double black hole evolution mechanisms on the mass ratio. The evolution of double black holes is divided into three stages: 1, the kinetic viscosity of each and the surrounding stars falls into the galaxy center; 2, the trisomy after the dynamic viscosity is not effective. In the second stages of the twin black hole evolution, if there is a co rotating gas accretion disk, the mass ratio of the double black holes in the center of the galaxy will be changed obviously in the early and late stages of the evolution of the double black holes, and the statistical distribution will be flat. We take different simulation results with the black in the combined Galaxy observed by SDSS. The results of the cavities are compared. The results of the principal and conditional p0.3 in the model are found to be in good agreement with the observation. On this basis, the effect of the confluent Accretion Disc is added to the statistical distribution of the mass ratio, and it is found that the mass ratio of the double black hole evolution will be more flat than the distribution, and the mass ratio is more than the distribution in the later period. A double black hole close to 1.
After the successful establishment of the cosmological evolution model of black hole and dark matter, we have also discussed the setting of space gravitational wave detector (ALIA) parameter space on this basis, in order to allow space detectors to limit the model and evolution of the Gao Hongyi black hole growth. In ALIA, the length of the arm is one order of magnitude smaller than that of LISA. In the case of reducing the requirement of the instrument, the ALIA can also make a good tool for the design of the medium quality double black hole and coincidence rate than that of LISA. More research on the gravitational wave source will be carried out in the future.
The cosmological parameters used in the model are as follows: QM=0.3, Omega A=0.7, h=0.7, bh2=0.02, 8=0.93 and n=1., where h is defined as H0=h * 100km s-1Mpc-1.
【學(xué)位授予單位】：中國(guó)科學(xué)技術(shù)大學(xué)
【學(xué)位級(jí)別】：博士
【學(xué)位授予年份】：2014
【分類號(hào)】：P145.8

【共引文獻(xiàn)】

相關(guān)期刊論文 前1條

1 楊愛華;;類星體形成的半解析模型[J];天文學(xué)報(bào);2014年01期

相關(guān)博士學(xué)位論文 前2條

1 郝景萌;伽瑪射線暴與恒星形成率的相關(guān)性研究[D];中國(guó)科學(xué)技術(shù)大學(xué);2013年

2 王煈;引力波天文學(xué)及數(shù)據(jù)處理相關(guān)問題[D];南京大學(xué);2013年

相關(guān)碩士學(xué)位論文 前1條

1 Gleniese E.McKenzie;[D];中國(guó)科學(xué)技術(shù)大學(xué);2014年

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本文編號(hào)：2014938