Theoretical Emission‐Line Profiles of Active Galactic Nuclei and the Unified Model. I. The Face‐on Torus

1997 ◽  
Vol 474 (2) ◽  
pp. 616-622 ◽  
Author(s):  
R. Quintilio ◽  
S. M. Viegas
Keyword(s):  
Emission Line ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Unified Model ◽  
Line Profiles ◽  
The Face

scholarly journals NEON AND $[{\rm{C}}\,{\rm{II}}]$ 158 μ m EMISSION LINE PROFILES IN DUSTY STARBURSTS AND ACTIVE GALACTIC NUCLEI

2016 ◽  
Vol 226 (1) ◽  
pp. 11 ◽  
Author(s):  
Anahit Samsonyan ◽  
Daniel Weedman ◽  
Vianney Lebouteiller ◽  
Donald Barry ◽  
Lusine Sargsyan
Keyword(s):  
Emission Line ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Line Profiles

Narrow emission-line profiles of active galactic nuclei

1989 ◽  
Vol 343 ◽  
pp. 78 ◽  
Author(s):  
M. Contini ◽  
S. M. Viegas-Aldrovandi
Keyword(s):  
Emission Line ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Line Profiles ◽  
Narrow Emission

scholarly journals Interacting Nuclei in Distant Galaxies

1990 ◽  
Vol 124 ◽  
pp. 251-253
Author(s):  
Wei Zheng ◽  
Steven A. Grandi
Keyword(s):  
Emission Line ◽  
Active Galactic Nuclei ◽  
Accretion Disk ◽  
Outer Part ◽  
Line Emission ◽  
Galactic Nuclei ◽  
Balmer Line ◽  
Line Profiles ◽  
Double Peaks ◽  
Distant Galaxies

The interaction of galaxies not only occurs in galactic scales, but also may be linked to the binary cores in active galactic galaxies. The presence of a binary in the center of galaxies was suggested by Begelman, Blandford and Rees (1980). Gaskell (1983) suggests that supermassive binaries may account for the observed structure of emission line profiles such as double peaks displaced by a significant velocity difference. Collin-Souffrin, et al. (1986) argue that line emission may be formed in the outer part of an accretion disk. The resultant profile, as expected from rotational motion, would be very broad and often possess a double-horn shape. However, the emission line profiles in most active galactic nuclei do not share such a resemblance, and there are only two reported cases, 3C390.3 (Pérez et al. 1987) and Arp102B (Chen, Halpern and Filippenko 1989), in which the broad Balmer line profile may be of such a shape. Therefore, the assumption for accretion disk is to be verified with care.

scholarly journals On the Time Scales of Optical Variability of AGN and the Shape of Their Optical Emission Line Profiles

Atoms ◽  
2019 ◽  
Vol 7 (1) ◽  
pp. 26
Author(s):  
Edi Bon ◽  
Paola Marziani ◽  
Predrag Jovanović ◽  
Nataša Bon
Keyword(s):  
Emission Line ◽  
Active Galactic Nuclei ◽  
Time Scales ◽  
Accretion Disks ◽  
Galactic Nuclei ◽  
Optical Emission ◽  
Light Curves ◽  
Optical Variability ◽  
Line Profiles ◽  
Line Shapes

The mechanism of the optical variability of active galactic nuclei (AGN) is still very puzzling. It is now widely accepted that the optical variability of AGN is stochastic, producing red noise-like light curves. In case they were to be periodic or quasi-periodic, one should expect that the time scales of optical AGN variability should relate to orbiting time scales of regions inside the accretion disks with temperatures mainly emitting the light in this wavelength range. Knowing the reverberation scales and masses of AGN, expected orbiting time scales are in the order of decades. Unfortunately, most of monitored AGN light curves are not long enough to investigate such time scales of periodicity. Here we investigate the AGN optical variability time scales and their possible connections with the broad emission line shapes.

scholarly journals Theoretical Narrow Emission-Line Profiles of Active Galactic Nuclei

1989 ◽  
Vol 134 ◽  
pp. 318-319
Author(s):  
M. Contini ◽  
S.M. Viegas-Aldrovandi
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Active Galactic Nuclei ◽  
Line Profile ◽  
Galactic Nuclei ◽  
Line Profiles ◽  
Narrow Emission

In recent years, a large number of high resolution observations of active galactic nuclei (AGN) have become available. Most of them show the [OIII]5007 line profile (Heckman, Miley and Green 1984, Vrtilek and Carleton 1985, Whittle 1985a,b).

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