Relevant bibliographies by topics / Supermassive Black Hole

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Academic literature on the topic 'Supermassive Black Hole'

Author: Grafiati
Published: 4 June 2021
Last updated: 25 February 2023

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Journal articles on the topic "Supermassive Black Hole"

1

Ganguly, Mekhala. "M87 Supermassive Black Hole Review." International Journal of Science and Research (IJSR) 10, no. 5 (2021): 896–99. http://dx.doi.org/10.21275/sr21521182804.

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2

Kelly, Brandon C., and Andrea Merloni. "Mass Functions of Supermassive Black Holes across Cosmic Time." Advances in Astronomy 2012 (2012): 1–21. http://dx.doi.org/10.1155/2012/970858.

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The black hole mass function of supermassive black holes describes the evolution of the distribution of black hole mass. It is one of the primary empirical tools available for mapping the growth of supermassive black holes and for constraining theoretical models of their evolution. In this paper, we discuss methods for estimating the black hole mass function, including their advantages and disadvantages. We also review the results of using these methods for estimating the mass function of both active and inactive black holes. In addition, we review current theoretical models for the growth of supermassive black holes that predict the black hole mass function. We conclude with a discussion of directions for future research which will lead to improvement in both empirical and theoretical determinations of the mass function of supermassive black holes.
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3

Davies, Melvyn B., Abbas Askar, and Ross P. Church. "The ecology of the galactic centre: Nuclear stellar clusters and supermassive black holes." Proceedings of the International Astronomical Union 14, S351 (2019): 80–83. http://dx.doi.org/10.1017/s1743921319006689.

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AbstractSupermassive black holes are found in most galactic nuclei. A large fraction of these nuclei also contain a nuclear stellar cluster surrounding the black hole. Here we consider the idea that the nuclear stellar cluster formed first and that the supermassive black hole grew later. In particular we consider the merger of three stellar clusters to form a nuclear stellar cluster, where some of these clusters contain a single intermediate-mass black hole (IMBH). In the cases where multiple clusters contain IMBHs, we discuss whether the black holes are likely to merge and whether such mergers are likely to result in the ejection of the merged black hole from the nuclear stellar cluster. In some cases, no supermassive black hole will form as any merger product is not retained. This is a natural pathway to explain those galactic nuclei that contain a nuclear stellar cluster but apparently lack a supermassive black hole; M33 being a nearby example. Alternatively, if an IMBH merger product is retained within the nuclear stellar cluster, it may subsequently grow, e.g. via the tidal disruption of stars, to form a supermassive black hole.
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4

Petri, A., A. Ferrara, and R. Salvaterra. "Supermassive black hole ancestors." Monthly Notices of the Royal Astronomical Society 422, no. 2 (2012): 1690–99. http://dx.doi.org/10.1111/j.1365-2966.2012.20743.x.

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5

SOHN, Bong Won. "Black Hole, Observed." Physics and High Technology 29, no. 12 (2020): 23–28. http://dx.doi.org/10.3938/phit.29.046.

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The author explains black holes in the context of astronomy and astrophysics. The history of black hole research and black hole discovery are covered briefly. The author explains why supermassive black holes in active galactic nuclei are the most promising candidates for imaging black holes. The principles of radio interferometers used as observation methods are covered. The Event Horizon Telescope Collaboration, its future plans, and the role of the Korean members are introduced.
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6

Jovanovic, P. "Investigation of some galactic and extragalactic gravitational phenomena." Serbian Astronomical Journal, no. 185 (2012): 1–16. http://dx.doi.org/10.2298/saj1285001j.

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Here we present a short overview of the most important results of our investigations of the following galactic and extragalactic gravitational phenomena: supermassive black holes in centers of galaxies and quasars, supermassive black hole binaries, gravitational lenses and dark matter. For the purpose of these investigations, we developed a model of a relativistic accretion disk around a supermassive black hole, based on the ray-tracing method in the Kerr metric, a model of a bright spot in an accretion disk and three different models of gravitational microlenses. All these models enabled us to study physics, spacetime geometry and effects of strong gravity in the vicinity of supermassive black holes, variability of some active galaxies and quasars, different effects in the lensed quasars with multiple images, as well as the dark matter fraction in the Universe. We also found an observational evidence for the first spectroscopically resolved sub-parsec orbit of a supermassive black hole binary system in the core of active galaxy NGC 4151. Besides, we studied applications of one potential alternative to dark matter in the form of a modified theory of gravity on Galactic scales, to explain the recently observed orbital precession of some S-stars, which are orbiting around a massive black hole at the Galactic center.
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7

DeGraf, Colin. "Supermassive black hole seed formation and the impact on black hole populations across cosmic time." Proceedings of the International Astronomical Union 15, S356 (2019): 292. http://dx.doi.org/10.1017/s1743921320003142.

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AbstractAlthough it is well understood that supermassive black holes are found in essentially all galaxies, the mechanisms by which they initially form remain highly uncertain, despite the importance that the formation pathway can have on AGN and quasar behaviour at all redshifts. Using a post-processing analysis method combining cosmological simulations and analytic modeling, I will discuss how varying the conditions for formation of supermassive black hole seeds leads to changes in AGN populations. Looking at formation via direct collapse or from PopIII remnants, I will discuss the impact on black hole mass and luminosity functions, scaling relations, and black hole mergers, which each have effects at both high- and low-redshifts. In addition to demonstrating the importance of initial seed formation on our understanding of long-term black hole evolution, I will also show that the signatures of seed formation suggest multiple means by which upcoming electromagnetic and GW surveys (at both high- and low-z) can provide the data required to constrain initial supermassive black hole formation.
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8

Jovanovic, Predrag, and Luka Popovic. "Supermassive binary black holes - possible observational effects in the x-ray emission." Facta universitatis - series: Physics, Chemistry and Technology 12, no. 2 (2014): 159–66. http://dx.doi.org/10.2298/fupct1402159j.

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Here we discuss the possible observational effects in the X-ray emission from two relativistic accretion disks in a supermassive binary black hole system. For that purpose we developed a model and performed numerical simulations of the X-ray radiation from a relativistic accretion disk around a supermassive black hole, based on the ray-tracing method in the Kerr metric, and applied it to the case of the close binary supermassive black holes. Our results indicate that the broad Fe K? line is a powerful tool for detecting such systems and studying their properties. The most favorable candidates for observational studies are the supermassive binary black holes in the galactic mergers during the phase when the orbital velocities of their components are very large and exceed several thousand kms -1.
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9

Chary, Ranga-Ram. "The spins of supermassive black holes." Proceedings of the International Astronomical Union 15, S356 (2019): 255. http://dx.doi.org/10.1017/s1743921320003051.

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AbstractWe present 1-second cadence, precise optical observations from SOFIA and Palomar of a sample of nearby supermassive black holes. The observations were taken to identify the shortest timescale variability in the nuclear photometry which may be associated with instabilities in the accretion flow in the immediate vicinity of the black hole. The shortest timescale variability, if associated with the radius of the innermost stable circular orbit (ISCO), can then be used to estimate the spin of the black hole. Despite 1% precision photometry, we obtained a non-detection of any significant variability in the nucleus of M32 (Mbh ∼ 2.5 × 106 Mȯ). Given the density of the stellar cusp, this argues for a scenario where 1000 Msun seed black holes formed from the coalescence of less massive black holes, which then accrete the gas produced by stellar interactions/winds. In more luminous systems however, we find a significant deection of variability and present hypotheses to explain the signal and thereby the origin of supermassive black holes.
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10

Dressler, Alan. "Observational Evidence for Supermassive Black Holes." Symposium - International Astronomical Union 134 (1989): 217–32. http://dx.doi.org/10.1017/s0074180900140914.

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A growing body of evidence from stellar dynamics in the nuclei of galaxies indicates that supermassive black holes of 107–109 M0 are common. The two best cases are M31 and M32, for which dark, central mass concentrations are the only straightforward interpretation. M87 continues to be a possible location of an even more massive black hole, but new observations and models by the author and D. Richstone effectively rule out the high black hole mass ∼5 × 109 M0 claimed by Sargent, Young, and collaborators. New data are available for several other nearby galaxies which also show kinematic signatures that could also be due to supermassive black holes. The Hubble Space Telescope will play the key role in strengthening these cases and eliminating, for the best examples, alternative models which do not require supermassive black holes.
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