Hostname: page-component-8448b6f56d-dnltx Total loading time: 0 Render date: 2024-04-25T00:47:35.131Z Has data issue: false hasContentIssue false
  • English
  • Français

Tidal Triggering of Seyfert Galaxies and Quasars: Physical Sufficiency

Published online by Cambridge University Press:  19 July 2016

G.G. Byrd ,
M.J. Valtonen ,
B. Sundelius  and
L. Valtaoja
G.G. Byrd
Affiliation:
Department of Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487 U.S.A.
M.J. Valtonen
Affiliation:
Department of Physical Sciences, University of Turku, Finland
B. Sundelius
Affiliation:
Onsala Space Observatory and Department of Astronomy, Chalmers University of Technology, Sweden
L. Valtaoja
Affiliation:
Department of Physical Sciences, University of Turku, Finland

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Excess optical and radio emission in nuclei of Seyfert galaxies and quasars is observationally related to nearby companions. Dahari found Seyferts are more strongly perturbed tidally by companions than normal spirals are. QSO data suggests a similar relationship. Quasar and Seyfert activity are thought to be fueled by gas inflow to the nucleus. To study whether gravitational tides from companions cause inflow from the spiral's disk, we use a self-gravitating 60,000 particle disk in Miller's polar n-body program. The perturbation to produce levels of inflow required for activity matches Dahari's Seyfert triggering level. QSO's are also perturbed by observed companions more than necessary for high inflow. We reanalyze Dahari's data to find that at least the majority of Seyferts are in multiple systems. Tidal triggering thus could be the main cause of Seyfert activity.

Type
Chapter VIII: Galaxies and Clusters
Information
Symposium - International Astronomical Union , Volume 124: Observational Cosmology , 1987 , pp. 527 - 530
Copyright
Copyright © Reidel 1987 

References

Balick, B., Heckman, T.M.: 1982, Ann. Rev. Astron. Astrophys. 20, 431.Google Scholar
Byrd, G.G., Saarinen, S., Valtonen, M.J.: 1986a, M.N.R.A.S., 220, 619.Google Scholar
Byrd, G.G., Valtonen, M.J., Sundelius, B., and Valtaoja, L.: 1986b, A. and A. 166, 75.Google Scholar
Byrd, G.G., Sundelius, B., and Valtonen, M.: 1987, A. and A. (in press).Google Scholar
Dahari, O.: 1984, A.J. 89, 966.Google Scholar
Dahari, O.: 1985, Ap. J. Supp. 57, 643.Google Scholar
Dahari, O.: 1985, A. J. 90, 1772.Google Scholar
Hutchings, J.B., Campbell, B.: 1983, Nature 303, 584.CrossRefGoogle Scholar
Keel, W.C., Kennicutt, R.C., Hummel, E., van der Hulst, J.M.: 1985, A.J. 90, 708.Google Scholar
Miller, R.H.: 1976, J. Comput. Phys. 21, 400.Google Scholar
Miller, R.H.: 1978, A.J. 224, 32.Google Scholar
Simkin, S.M., Su, H.J., Schwarz, M.P.: 1980, Ap. J. 237, 404.Google Scholar
Stockton, A.: 1982, Ap. J. 257, 33.Google Scholar
Toomre, A. and Toomre, J.: 1972, Ap. J., 178, 623.Google Scholar