PPT-The nature of the accretion flow in AGN

Author : ximena | Published Date : 2024-02-09

Prof Chris Done University of Durham amp ISASJAXA AGN feedback MagorrianGebhardt relation gives BH mass Big black holes live in host galaxies with big bulges Either

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The nature of the accretion flow in AGN: Transcript

Prof Chris Done University of Durham amp ISASJAXA AGN feedback MagorrianGebhardt relation gives BH mass Big black holes live in host galaxies with big bulges Either measured by bulge luminosity or bulge mass stellar velocity dispersion or . . Statistics. : . 1.8 . Ms. ½. . sq. .deg. . @. 160 . ksec. 1761 . sources. Dec. ’06-June ’07. Catalog. : . Elvis . et. al., . 2009, ApJS 184, 158. Martin Elvis, Francesca . Civano. , . Aldcroft. between . XRB. and . AGN. . Accretion . Processes. Anca. . Constantin. James Madison Univ.. W/. Paul . Green(SAO. ) . Tom . Aldcroft. (SAO. ). HongYan. . Zhou(USTChina. ). Daryl Haggard (. UWashington. Neutron Star Binaries and Its Implications. QCS2014@2014.10.20. Chang-Hwan Lee @. 1. Nuclear Physics A 928 (2014) 296. (. 李昌桓. ). Prakash (2013). All well measured NS masses in NS-NS binaries are < 1.5 . JWST Workshop. – . STScI. Baltimore. June 8, 2011. Mid-Infrared Observation of High . Redshift. Galaxy Evolution. Most star formation activity occurs behind dust . Chary & Pope . 2011. Bouwens. Tori. : . Theory & Observations. Moshe . Elitzur. . University of Kentucky . Unified Scheme for AGN. M. . ~ 10. 6 . – 10. 10. M. . R. s. ~ 10. 11 . – 10. 15 . cm. T. oroidal. and . Galaxy Evolution. Meg Urry. Yale University. ~All galaxies host supermassive black holes. The . formation. and . evolution. of . galaxies. is closely tied to. the . growth. of . black holes. Smolcic. . ea. ). Compilation based on different star formation estimators (UV, IR, radio, Hα..). Large scatter: Dust obscuration is major problem. Hopkins & . Beacom. (2006) compilation. redshift. は階層的銀河形成論で説明. できるか？. Motohiro. 　. Enoki. Tomoaki Ishiyama (Tsukuba Univ.). Masakazu A. R. Kobayashi (Ehime Univ.). Masahiro . Nagashima. . (Nagasaki Univ. .). §1. Introduction. Andrei LobanovMPIfR, Bonn AGN/RG ScienceAGN/RG Science AGN/RG drivers for LOFAR and SKA: astrophysical masers, nuclear regions of AGN, physics of relativistic and mildly relativistic outflows, kinetic Electra . Panagoulia. Institute of Astronomy, Cambridge, UK. W. ith: Andy Fabian. Jeremy Sanders. Julie . Hlavacek-Larrondo. X-ray View of Galaxy Ecosystems . 11. th. July 2014. . GIOVANNOLI. Laboratoire. . d’Astrophysique. de Marseille, FRANCE. Advisor : Veronique BUAT. C. ollaborators. : Denis . Burgarella. , Stefan Noll. Spectral . energy. distribution . modeling. . Hee. -Won Lee. Department of Physics and Astronomy. Sejong. University. 2015. 1. 27. Content. Introduction. Scattering . and Unification of AGN. Scattered Ly . alpha. Balmer. Wings. Discussion. Active Galactic Nuclei. VG. So we want a color magnitude diagram for AGN so that by looking at the color of an AGN we can get its luminosity. But AGN have no fusion, why would we expect a color-magnitude relation?. The gas that accretes onto the black hole is still hot and so must follow the Blackbody Radiation law. . Aggregate Analysis In A CubeSat Centrifuge: A Study Of Primary Accretion Sarah Smallwood Faculty Mentor: Erik Asphaug , School of Earth and Space Exploration Graduate Student Mentor: Elizabeth Dyer

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