Hostname: page-component-78c5997874-ndw9j Total loading time: 0 Render date: 2024-11-06T10:09:21.651Z Has data issue: false hasContentIssue false
  • English
  • Français

Dusty, radiation pressure dominated photoionization: The solution to the narrow line region problem

Published online by Cambridge University Press:  24 November 2004

Brent Groves ,
Michael Dopita  and
Ralph Sutherland
Brent Groves
Affiliation:
Research School of Astronomy & Astrophysics, Australia National University, Canberra, Australia email: [email protected]
Michael Dopita
Affiliation:
Research School of Astronomy & Astrophysics, Australia National University, Canberra, Australia email: [email protected]
Ralph Sutherland
Affiliation:
Research School of Astronomy & Astrophysics, Australia National University, Canberra, Australia email: [email protected]
Rights & Permissions [Opens in a new window]

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.

Seyfert narrow line regions (NLR) have emission line ratios which are remarkably uniform, displaying only ∼0.5 dex variation between different galaxies. Existing models have been unable to explain these observations without the introduction of ad hoc assumptions, geometrical restrictions or new parameters. Here we introduce a new model: dusty radiation pressure dominated photoionization, which provides a natural self-regulating characteristic, leading to an invariance of the spectrum over a very wide range (>100) of ionization parameter. The dusty model is able to reproduce both the range and the absolute value of the observational line ratios not only in the standard optical diagnostic diagrams but also in UV diagnostic plots, providing an explanation to the problem in NLR observations.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
ORAL CONTRIBUTIONS
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS222 , March 2004 , pp. 263 - 266
Copyright
© 2004 International Astronomical Union