Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21336101f&link_type=abstract
American Astronomical Society, AAS Meeting #213, #361.01; Bulletin of the American Astronomical Society, Vol. 41, p.510
Astronomy and Astrophysics
Astronomy
Scientific paper
A subset of Active Galactic Nuclei (AGNs) have broad, double-peaked Balmer emission lines, regarded as the best kinematic evidence for the production of broad lines by the accretion disk. It has been suggested that double-peaked emitters have a weak or non-existent disk-wind, hence offering a direct view of the accretion disk. Thus, the variability of the double-peaked line profile, which is uncorrelated with variations of the continuum flux traces changes in the structure of the accretion disk. We analyze the line profile variability of 10 double-peaked emitters, extending the luminosity range of previous variability studies. We use the line profile variability to probe the accretion disk structure and find evidence that the line-emitting region of the accretion disk is partially or totally unstable to self-gravity. We also argue that the double-peaked emitters are connected to the single-peaked emitters since radiative transfer effects through a disk-wind can significantly alter the emission line profile. This suggests very strongly that our results about the accretion disk structure can be generalized to the entire population of AGNs.
Eracleous Michael
Flohic Helene
No associations
LandOfFree
Interpreting Double-Peaked Emission Line Profile Variability in AGNs usingModels for Accretion Disk Structures does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Interpreting Double-Peaked Emission Line Profile Variability in AGNs usingModels for Accretion Disk Structures, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Interpreting Double-Peaked Emission Line Profile Variability in AGNs usingModels for Accretion Disk Structures will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1700800