Long Term Profile Variability of Double-Peaked Emission Lines in AGNs

Details Long Term Profile Variability of Double-Peaked Emission Lines in AGNs Long Term Profile Variability of Double-Peaked Emission Lines in AGNs

2003-09-23

arxiv.org/abs/astro-ph/0309624v1

Astronomy and Astrophysics

Astrophysics

4 pages, 1 figure, uses newpasp.sty To appear in "AGN Physics with the Sload Digital Sky Survey" Princeton, July 27-30, 2003

Scientific paper

An increasing number of AGNs exhibit broad, double-peaked Balmer emission lines, which are thought to arise from the outer regions of the accretion disk which fuels the AGN. The line profiles are observed to vary on a characteristic timescales of 5-10 years. The variability is not a reverberation effect; it is a manifestation of physical changes in the disk. Our group has monitored a set of 20 double-peaked emitters for the past 8 years (longer for some objects). Here, we characterize the variability of the double-peaked H alpha line profiles in five objects from our sample. By experimenting with simple models, we find that disks with a single precessing spiral arm are able to reproduce many of the variability trends that are seen in the data.

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