3 edition of Accretion disks, precessing jets, and the asymmetric emission lines of QSOs found in the catalog.
Accretion disks, precessing jets, and the asymmetric emission lines of QSOs
|Series||NASA-CR -- 173632, NASA contractor report -- 173632|
|Contributions||United States. National Aeronautics and Space Administration|
|The Physical Object|
ASTR Practice questions for lecture Accretion Disks 1. Show that for a particle in a Newtonian orbit with a given angular momentum, the lowest-energy state is a circular orbit. This motivates the claim that dissipation will tend to put ﬂuid elements into nearly-circular orbits. 2. Do a toy problem to determine whether accretion can. The observed iron Kα fluorescence lines in Seyfert I galaxies provide strong evidence for an accretion disk near a supermassive black hole as a source of the line emission. Here we present an analysis of the geometrical and kinematic properties of the disk based on the extreme frequency shifts of a line profile as determined by the measurable flux in both the red and blue Author: Vladimir I. Pariev, Benjamin C. Bromley, Warner A. Miller.
•Hydromagnetic flows from accretion discs and the production of radio jets”, Blandford & Payne •“Magnetically driven jets and winds: Exact solutions”, Contopoulos & Lovelace •“A simple type of magnetically driven jets: an astrophysical plasma gun”, Contopoulos This book highlights selected topics of standard and modern theory of accretion onto black holes and magnetized neutron stars. The structure of stationary standard discs and non-stationary viscous processes in accretion discs are discussed to the highest degree of accuracy analytic theory can provide, including relativistic effects in flat and warped discs around black holes.
INTRODUCTION. Galaxies with core luminosities of about 10 42 erg s − 1 fall at the borderline between nuclear starbursts and active galactic nuclei (AGN). When identified as AGN they often share a number of common features: extended radio lobes and often collimated jets, and an emission-line spectrum dominated by low-excitation lines often associated with an Cited by: Outflows are ubiquitous in active galactic nuclei (AGN). They can take the form of either dramatic radio jets, which extend vast distances into the inter-galactic medium, or of much smaller scale winds - whose existence can be inferred only indirectly via their influence on the observed spectra. There is good evidence to show that winds are likely to arise from the accretion disks Author: Nicholas Higginbottom.
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Get this from a library. Accretion disks, precessing jets, and the asymmetric emission lines of QSOs. [G A Shields; United States. National Aeronautics and Space Administration.]. ACCRETION DISK TEMPERATURES OF QSOs: CONSTRAINTS FROM THE EMISSION LINES E.
Bonning1,2, G The idea of accretion disks around supermassive black holes as the power source of active galactic nuclei (AGN) is widely Physical plausibility, the lack of successful alterna-tives, and the frequent presence of bipolar jets support this picture.
Unusual emission lines are observed that cannot be identified except as high-velocity ( km s-1) bipolar outflows or jets. These outflows are seen in H and He II at the same positive and. are AGN. The integral emission of AGN reﬂects the history of accretion onto SMBH over cosmic time.
Emission lines are usually seen in the X-ray spec-tra of AGN. The broad emission Fe Kα spectral line (– keV, depending on ionization state) with. Eddington Accretion and QSO Emission Lines at z ~ 2. accretion results in geometrically thic k accretion disks whic h.
it difficult to. Binary Black Holes, Accretion Disks and Relativistic Jets: Photocenters of Nearby AGN and Quasars Principal Investigator: Ann E. Wehrle (Interferometry Science Center/JPL/Caltecli) Team Members: Dayton L.
Jones (JPL), David Meier (JPL), B. Glenn Piner (Whittier College), Stephen C. Unwin (JPL) One of the most challenging questions in astronomy today is to understand the File Size: 2MB. emission. Stratiﬁed MHD disk winds could therefore serve as a unique means to understand and unify the diverse AGN outﬂows.
Key words: accretion, precessing jets disks – black hole physics – galaxies: active – quasars: absorption lines – X-rays: galaxies Online-only material: color ﬁgures 1.
INTRODUCTION. The accretion disc grows until a steady state, where the gas that reach it is equal to that falling into the black hole.
The friction will heat the gas to extremely high temperatures. The accretion disc will glow in the x-ray portion of the spectrum. The matter in. This book provides a comprehensive picture of the formation of stars and planetary systems, from their beginnings in cold clouds of molecular gas to their emergence as new suns with planet-forming disks.
At each stage gravity induces an inward accretion of mass, and this is a central theme for the book. The author brings together current Cited by: An important reason precessing jets were not discovered earlier is that 3-D simulations of the region surrounding a rapidly spinning black hole require an enormous amount of computational power.
Calaclysmic variables (white dwarf accretors) – accretion from binary companion – winds AGN – accretion from environment – winds & jets Galactic black holes/neutron stars – accretion from companion – winds jets Gamma-ray bursts – winds & jets Many astronomical systems with accretion disks develope jets.
But not all. an accretion disk. In nova-like and dwarf novae in outburst, the disk is the main source of radiation. The inner disk emission dominates the ultraviolet (UV) spectrum (Warner ). Several efforts have been made to understand the spectral features of Cited by: 9. An astrophysical jet is an astronomical phenomenon where outflows of ionised matter are emitted as an extended beam along the axis of rotation.
When this greatly accelerated matter in the beam approaches the speed of light, astrophysical jets become relativistic jets as they show effects from special relativity.
The formation and powering of astrophysical jets are highly complex. title = "Coronal accretion: The power of X-ray emission in AGN", abstract = "The optical/UV and X-ray emissions in luminous AGN are commonly believed to be produced in an accretion disk and an embedded hot corona : B.-F.
Liu, R. Taam, E. Qiao, W. Yuan. DOUBLE- (AND SINGLE-) PEAKED EMISSION LINES AS PROBES OF THE STRUCTURE OF THE OUTER ACCRETION DISKS IN AGN H. Flohic1 and M. Eracleous1 Broad, double-peaked Balmer emission lines provide dynamical evidence for the presence of an accretion disk feeding a supermassive black hole in the central engines of AGN.
synthesis of emission lines; and ﬁnally in Sect. 4 we drawn our conclusions. The Model The model describes a fragmented accretion stream impacting onto the surface of a CTTS. We assume that the accretion occurs along magnetic ﬁeld lines that link the circumstellar disk to the surface of the star, and that the accretion stream is not Cited by: Observations are providing increasingly detailed quantitative information about the accretion flows that power such high energy systems as X-ray binaries and Active Galactic Nuclei.
These observations have been modeled in some detail by a variety of accretion scenarios, but such models rely on unavoidable assumptions such as regular flow geometry and a simple, Cited by: Analyses are given of various processes involving matter falling into or coming out of black holes.
A significant amount of matter may fall into a black hole in a galactic nucleus or in a binary system. There gas with relatively high angular momentum is expected to form an accretion disk flowing into the hole. In this thesis the conservation laws of rest mass, energy, and angular Cited by: 7.
Accretion Disks aroundBlack Holes • optically thin advection-dominated ﬂows • mass loss and jets • super-Eddington accretion APP4: Ultraluminous X-Ray Sources ⊲ stellar versus intermediate-mass black holes ⊲ photon bubble instabilities APP5: Active Galactic Nuclei ⊲ characteristic properties ⊲ black-hole growth.
Experimental determination of the threshold luminosity above which the instability is activated gave % of Eddington Luminosity, depending on binary parameters.
The instability may provide a suitable mechanism for causing accretion disks to tilt out of the binary plane, thereby causing them to start : J. Petterson, J. Petterson, J. Greenberg, J. Greenberg, R. Iping, R. Iping. Accretion Power in Astrophysics examines accretion as a source of energy in both binary star systems containing compact objects, and in active galactic nuclei.
Assuming a basic knowledge of physics, the authors describe the physical processes at work in accretion discs and other accretion by: You are being redirected.The Broad-Line Region in Active Galactic Nuclei B.M.
Peterson Department of Astronomy, The Ohio State University, West 18th Avenue, Columbus, OHUSA [email protected] Abstract. We review the basic observed and inferred properties of the broad emission-line region in AGNs, as well as the basics of the .