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Optical Spectrum Variability of Seyfert Galaxy Nuclei

Published online by Cambridge University Press:  30 March 2016

A. G. de Bruyn
A. G. de Bruyn*
Affiliation:
Hale Observatories, California Institute of Technologyand, Carnegie Institution of Washington, and, Netherlands Foundation for Radio Astronomy, Dwingeloo

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In this contribution I will present some results of a program aimed at determining the optical variability characteristics of Seyfert galaxy nuclei. It has been known for more than a decade that the continuous, non-stellar light of Seyfert nuclei can vary significantly on a time scale of months to years (see, e.g., Lyutyi, 1973, 1977; Penston et al., 1974; Penfold, 1979). In recent years there also have been various reports of variations in the intensity of the broad optical emission lines (Boksenberg and Netzer, 1977; Tohline and Osterbrock, 1976) following the pioneering work by Souffrin et al. (1973) and Cherepashchuk and Lyutyi (1973). However, very little is known on the details of the continuum variations and how they relate to the line variability. Such information could provide valuable constraints on the fashionable photo-ionization models for the broad line region (BLR) and the structure of the latter.

Type
Joint Discussion
Information
Highlights of Astronomy , Volume 5: Highlights of Astronomy. As presented at the XVIIth General Assembly of the IAU, 1979 , 1980 , pp. 631 - 639
Copyright
Copyright © Cambridge University Press 1980

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