Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21832717f&link_type=abstract
American Astronomical Society, AAS Meeting #218, #327.17; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
It is well known from the past optical/EUV observations that a small population of AGNs exhibits the so called broad double-peaked Balmer line profiles (FWHM 10,000 km/sec); i.e. 20% of the radio-galaxies (RGs) and radio-loud (RL) AGNs at z<0.4 while only 3-4% of SDSS AGNs at z<0.33 (e.g. Arp 102B and 3C 390.3). Its theoretical interpretation has been based on a Keplerian accretion disk where line photons are Doppler-shifted due to rotation to form the broadened red/blue tails although the predicted line strength is critically smaller than the observed intensity. As an alternative explanation to resolve this issue, we propose that magnetically-driven disk-winds can self-consistently reproduce both i) broad double-peaked line shape and ii) its normalization for many observed objects including those with single-peaked profiles. Our preliminary results suggest that the apparent spectral distinction in various Balmer lines can be accounted for by the wind structure as well as viewing angle. This line emission model is a continuation of our earlier work on absorption lines for Seyfert AGNs and BAL quasars, and we here demonstrate how both spectral signatures can be explained within this single disk-wind scenario.
Behar Ehud
Contopoulos Ioannis
Fukumura Keigo
Kazanas Demos
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