Radiative transfer in the broad emission line regions of quasi-stellar objects

1988 ◽  
Vol 331 ◽  
pp. 211 ◽  
Author(s):  
Eugene H. Avrett ◽  
Rudolf Loeser
Keyword(s):  
Radiative Transfer ◽  
Emission Line ◽  
Stellar Objects ◽  
Broad Emission ◽  
Quasi Stellar Objects ◽  
Broad Emission Line

scholarly journals Near infrared hydrogen emission line ratios as diagnostics of the broad emission line region

2012 ◽  
Vol 372 ◽  
pp. 012069
Author(s):  
Andrea J Ruff ◽  
David J E Floyd ◽  
Kirk T Korista ◽  
Rachel L Webster ◽  
Ryan L Porter ◽  
...  
Keyword(s):  
Emission Line ◽  
Near Infrared ◽  
Hydrogen Emission ◽  
Broad Emission ◽  
Line Region ◽  
Broad Emission Line ◽  
Hydrogen Emission Line

scholarly journals Broad emission line variability in 3C 273 *

1989 ◽  
Vol 240 (4) ◽  
pp. 741-751 ◽  
Author(s):  
P. T. O'Brien ◽  
W. Zheng ◽  
R. Wilson
Keyword(s):  
Emission Line ◽  
Broad Emission ◽  
Broad Emission Line

scholarly journals The X-SHOOTER/ALMA Sample of Quasars in the Epoch of Reionization. I. NIR Spectral Modeling, Iron Enrichment, and Broad Emission Line Properties

2020 ◽  
Vol 905 (1) ◽  
pp. 51
Author(s):  
Jan-Torge Schindler ◽  
Emanuele Paolo Farina ◽  
Eduardo Bañados ◽  
Anna-Christina Eilers ◽  
Joseph F. Hennawi ◽  
...  
Keyword(s):  
Emission Line ◽  
Spectral Modeling ◽  
Iron Enrichment ◽  
Broad Emission ◽  
Broad Emission Line

scholarly journals Star Clusters in Quasars: Bloated Stars as Broad Emission Line Clouds

1989 ◽  
Vol 134 ◽  
pp. 137-138
Author(s):  
R. C. Puetter
Keyword(s):  
Black Hole ◽  
Emission Line ◽  
Star Clusters ◽  
Hole Formation ◽  
Line Radiation ◽  
Black Hole Formation ◽  
Broad Emission ◽  
Broad Emission Line

Many scenarios of the evolution of star clusters in the centers of galaxies involve the formation of a central supermassive object. Since black hole formation is not 100% efficient in mass usage, stars are left over. This paper investigates the properties of such stars and proposes that their externally heated atmospheres become “bloated” due to radiative forces from trapped line radiation. Such stars would swell to many times their normal diameters and acquire densities, sizes, and mean column masses typical of QSO/AGN emission line clouds (ELCs).

scholarly journals Velocity Diagnostics of the Broad Emission-Line Region of Active Galactic Nuclei

1997 ◽  
Vol 159 ◽  
pp. 175-178 ◽  
Author(s):  
Brian Espey
Keyword(s):  
Emission Line ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Nuclear Region ◽  
Driving Mechanisms ◽  
Broad Emission ◽  
Line Region ◽  
Broad Emission Line ◽  
Ongoing Project

AbstractWe present a brief review of emission-line velocity differences, and describe an ongoing project to determine the driving mechanisms responsible. We conclude with a brief outline of the use of velocity differences as probes of the conditions in the nuclear region of AGNs.

scholarly journals Hidden Blazars In Radio Loud Quasars?

2000 ◽  
Vol 195 ◽  
pp. 411-412
Author(s):  
F. Ma
Keyword(s):  
Emission Line ◽  
Star Model ◽  
Broad Emission ◽  
Broad Emission Line ◽  
Initial Results

We present the initial results from our search for hidden blazars via CIV emission line variability among radio loud quasars. The implications on models of quasar Broad Emission Line Regions are discussed, and we focus on the tidally disrupted star model.

scholarly journals The Nature and Origin of Structure in Broad Emission Line Profiles

1997 ◽  
Vol 159 ◽  
pp. 193-194 ◽  
Author(s):  
C. Martin Gaskell ◽  
Stephanie A. Snedden
Keyword(s):  
Emission Line ◽  
The Other ◽  
Central Component ◽  
Balmer Line ◽  
Line Profiles ◽  
Broad Emission ◽  
Broad Emission Line

AbstractWe postulate that all structure in broad lines can be explained by a central component (at the systemic redshift) and the addition of two ‘displaced components’, one blueshifted and the other redshifted. We have been able to successfully classify all Balmer-line profiles on this basis. 3C 390.3-type objects are merely examples where the shifts of the displaced components are unusually large. We believe that the displaced peaks are less prominent in the UV lines because the higher ionization lines are broader.

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