Models For The Variability Of Double-peaked Emission Lines And Extension To Single-peaked Emission Lines

Details Models For The Variability Of Double-peaked Emission Lines And Extension To Single-peaked Emission Lines Models For The Variability Of Double-peaked Emission Lines And Extension To Single-peaked Emission Lines

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21110802f&link_type=abstract

American Astronomical Society, AAS Meeting #211, #108.02; Bulletin of the American Astronomical Society, Vol. 39, p.936

Astronomy and Astrophysics

Astronomy

Scientific paper

We explore the impact of a stochastically clumpy accretion disk structure on the profile variability of double-peaked emission lines observed in Active Galactic Nuclei (AGNs). We construct model line profiles from disks with a variety of clump distributions (with and without shearing). We compare the computed line profiles and their variability to 35 observations of 3C 390.3 and 91 observations of Arp 102B spanning at least 16 years. The comparison is carried out statistically in Fourier space. We find that clumps need to be clustered in the outer parts of the line emitting region to match the observations, favoring clump production through gravitational collapse. We also explore the effect of radiative transfer of line photons in a disk wind, by including relativistic effects and a varying emissivity function to previous models. High optical depth winds produce single-peaked profiles, as shown by previous models, and also with reduced variability as we find in our own models. This suggests that the small frequency of occurrence of double-peaked emission lines could be due to a high opacity wind modifying the line shape instead of different geometry and kinematics of the broad line region. In such a case, lessons from double-peaked emitters can applied to the general AGN population.

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