本文選題：超大質(zhì)量黑洞 + 射電干涉�。� 參考：《南京大學(xué)》2017年博士論文

【摘要】：超大質(zhì)量黑洞的吸積與反饋活動(dòng)是天體物理中重要的物理過(guò)程。超大質(zhì)量黑洞作為活動(dòng)星系核的引擎,通過(guò)吸積周圍的物質(zhì)將引力能轉(zhuǎn)換為輻射能,通過(guò)噴流、外流或者風(fēng)的形式向星際介質(zhì)反饋機(jī)械能。寄主星系和其中心黑洞無(wú)時(shí)不進(jìn)行著相互作用共同演化。因此,了解黑洞的吸積和反饋的物理過(guò)程是了解星系的形成與演化中重要的一環(huán)。但目前對(duì)超大質(zhì)量黑洞的吸積和反饋的物理過(guò)程并不清楚,這也一直是天體物理中的關(guān)鍵問(wèn)題。近幾十年來(lái),對(duì)于超大質(zhì)量黑洞的的觀測(cè)取得了很多進(jìn)展,例如：通過(guò)近鄰星系的巡天發(fā)現(xiàn)低光度活動(dòng)星系核在近鄰活動(dòng)星系核的樣本中占有很大的比例；在這些低光度活動(dòng)星系核中常常能觀測(cè)到核區(qū)致密的X射線和射電輻射；以及發(fā)現(xiàn)這些源常常在多波段存在光變。根據(jù)黑洞的觀測(cè)性質(zhì)(多波段觀測(cè)結(jié)果組成的寬帶能譜分布,磁場(chǎng)等),人們逐步建立了黑洞吸積在輻射模式和噴流史瓦西模式下不同的理論框架。然而,這一框架中依舊有很多關(guān)鍵問(wèn)題沒(méi)有得到解決,例如：是否超大質(zhì)量黑洞的射電輻射總有噴流的貢獻(xiàn),或者是否噴流的輻射主導(dǎo)著黑洞在射電波段的輻射？是否噴流進(jìn)行地方向會(huì)在演化中發(fā)生變化？以及在黑洞附近產(chǎn)生耀變的物理意義是什么？本論文通過(guò)對(duì)距離很近的三個(gè)星系M31,M 32和M 104中心的低光度活動(dòng)星系核的高分辨率的射電干涉陣的觀測(cè),討論了以下兩個(gè)問(wèn)題：1)吸積極不活躍的超大質(zhì)量黑洞的射電輻射性質(zhì)；2)盤星系中噴流對(duì)星際介質(zhì)的能量反饋。對(duì)這兩個(gè)問(wèn)題的研究可以給理論模型更多實(shí)際例子上的限制,從而進(jìn)一步了解黑洞活動(dòng)的物理過(guò)程。第二章中,我們通過(guò)使用Karl G. Jansky Very Large Array (JVLA)甚大陣射電干涉儀對(duì)M 31*進(jìn)行了多歷元的多波段的pc尺度的觀測(cè)。我們分析了這些連續(xù)譜觀測(cè)的結(jié)果,首次在10,15和20 GHz頻率探測(cè)到致密的射電核,并且看到在6 GHz的圖像中的致密的射電核周圍存在沿著不同方向的延展結(jié)構(gòu)。在2011到2012年問(wèn)多次的觀測(cè),看到了M 31*的流量在6 GHz頻率的流量變化,最短變化時(shí)標(biāo)在6小時(shí)內(nèi)出現(xiàn)了近40%的變化幅度,說(shuō)明光變可能來(lái)自～20個(gè)史瓦西半徑處。通過(guò)我們?cè)诙囝l率的觀測(cè)結(jié)果,我們建立了6到20 GHz的譜能量分布,擬合(Sv,∝ α)得到譜指數(shù)α～-0.45,并由此推斷射電輻射很可能是由噴流主導(dǎo)的。第三章中,M 32作為本星系群中的一個(gè)橢圓星系,其中心的超大質(zhì)量黑洞是最近的超大的質(zhì)量黑洞之一。我們利用JVLA干涉陣第一次探測(cè)到位于M 32星系核中心的一個(gè)致密射電源。這個(gè)射電源在中心頻率6.6 GHz的流量密度是～47.3±6.1 μJy。我們討論了這個(gè)射電源起源的可能性,認(rèn)為它起源于超大質(zhì)量黑洞的射電輻射。同時(shí)我們利用Chandra和XMM-Newton的X射線數(shù)據(jù)研究了這個(gè)超大質(zhì)量黑洞的X射線輻射性質(zhì)。第四章中,M 104 (NGC 4594)是一個(gè)大質(zhì)量的的早型旋渦星系,也被稱作草帽星系,在其中心存在一個(gè)原型的低光度活動(dòng)星系核。我們使用JVLA對(duì)M104在多波段進(jìn)行了不同分辨率的連續(xù)譜觀測(cè)以獲得其噴流在不同物理尺度的特征。通過(guò)分析認(rèn)為M 104的kpc尺度的延展很可能來(lái)自pc尺度的射電噴流。并且發(fā)現(xiàn)kpc尺度噴流的方向與pc尺度噴流的方向有差異,暗示了噴流在傳播過(guò)程中發(fā)生偏折,或者不同尺度的噴流產(chǎn)生自中心黑洞的不同活躍期；我們通過(guò)定量測(cè)量了kpc尺度噴流的磁壓,發(fā)現(xiàn)其與星際熱氣體的壓強(qiáng)相當(dāng),暗示了噴流在傳播過(guò)程中的機(jī)械功對(duì)氣體注入了可觀的能量。第五章中,我們主要介紹了對(duì)本論文工作的總結(jié)以及展望。
[Abstract]:The accretion and feedback activity of a supermassive black hole is an important physical process in astrophysics. As the engine of the active galactic nucleus, the supermassive black hole converts the gravitational energy into radiant energy by accretion of the surrounding material, and feedback the mechanical energy to the interstellar medium by the form of jet, outflow or wind. The host galaxy and its central black hole are all the time. The physical process of understanding the accretion and feedback of a black hole is an important link in understanding the formation and evolution of galaxies. However, the physical process of the accretion and feedback of a supermassive black hole is not clear at present. It is also a key problem in astrophysics. In recent decades, the supermassive black hole has been found. A lot of progress has been made, for example: a large proportion of the low photometric active galactic nuclei in the near adjacent active galactic nuclei is found through a cruise of near neighbor galaxies; the dense X rays and radio radiation of the nuclear region are often observed in these low photometric active galactic nuclei; and it is found that these sources often exist in multiple bands. According to the observational properties of the black hole (the broadband energy spectrum distribution, magnetic field, etc.), a different theoretical framework for the black hole accretion in the radiation pattern and the jet schwarzsche model is gradually established. However, there are still many key problems in this framework, such as whether the supermassive black hole is shot. Electrical radiation always has the contribution of jet flow, or whether or not the radiation of the jet dominates the radiation of the black hole in the radio band? Is the jet changing in the evolution? And what is the physical significance of the variation near the black hole? This paper passes the low luminosity stars of the three galaxies, M31, M 32, and M 104, which are very close to the distance. The observation of the high resolution radio interference array of the nucleus discusses the following two problems: 1) the radio radiation properties of the extremely inactive supermassive black holes; 2) the energy feedback of the jet on the interstellar medium in the disk galaxy. The study of these two problems can give more practical examples of the theoretical model, thus further understanding the black. In the second chapter, we observe M 31* by using Karl G. Jansky Very Large Array (JVLA) very large array radio interferometer to observe M 31* multispectral PC scales. We analyze the results of these continuous spectral observations, detect the dense radio nuclei for the first time in 10,15 and 20 GHz frequencies, and see in 6 The dense radio nucleus in the Z image has a ductile structure along different directions. From 2011 to 2012, the flow of the M 31* flow at 6 GHz frequency changes, and the shortest change is marked in 6 hours, which shows that the change may come from the 20 schwarzschi radius. The spectral energy distribution of 6 to 20 GHz is established by multi frequency observations. The spectral exponent alpha to -0.45 is obtained by fitting (Sv), and it is concluded that radio radiation is likely to be dominated by the jet. In the third chapter, M 32 is an elliptical galaxy in the cluster of galaxies, and the supermassive black hole in the center is one of the most recent supermassive black holes. We used the JVLA interference array for the first time to detect a dense radio source at the center of the M 32 nucleus. The discharge density of the source at the center frequency 6.6 GHz is 47.3 + 6.1 mu Jy.. We discuss the possibility of the origin of the emitter source. It is believed that it originated from the radio radiation of the supermassive black hole. At the same time, we use Chandra and XMM. The X ray data of -Newton studies the X ray radiation properties of the supermassive black hole. In the fourth chapter, M 104 (NGC 4594) is a large mass of early vortex galaxies, also known as the straw hat galaxies, and there is a prototype low photometric active galactic nucleus in its center. We have made JVLA to M104 in multiple bands with different resolutions. It is believed that the extension of the KPC scale of M 104 is likely to come from the radio jet of the PC scale through analysis, and it is found that the direction of the KPC scale jet is different from the direction of the PC scale jet, suggesting that the jet is deflected during the propagation process, or the jet of different scales is produced from the jet. At the different active stages of the central black hole, we measured the magnetic pressure of the KPC scale jet quantitatively, and found that it was equal to the pressure of the interstellar hot gas, suggesting that the mechanical work of the jet in the process of propagation has injected considerable energy into the gas. In the fifth chapter, we mainly introduce the summary and Prospect of the work in this paper.

【學(xué)位授予單位】：南京大學(xué)
【學(xué)位級(jí)別】：博士
【學(xué)位授予年份】：2017
【分類號(hào)】：P161;P152

【參考文獻(xiàn)】

相關(guān)期刊論文 前1條

1 C.Ke-shih Young;Malcolm J.Currie;Robert J.Dickens;;A Critical Review of the Evidence for M32 being a Compact Dwarf Satellite of M31 rather than a More Distant Normal Galaxy[J];Chinese Journal of Astronomy and Astrophysics;2008年04期

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本文編號(hào)：1877497