The efficiency of the Bowen fluorescence mechanism in models
of planetary nebulae and Seyfert galaxy nuclei has been calculated
by solving the equation of transfer for He II Ly -o( and the Bowen
lines using the Feautrier method. The calculated efficiencies, which
do not show significant differences between planetary nebulae and
Seyfert galaxies, range from about 40% to 50% for realistic models.
These values are somewhat higher than recent empirical determinations
of Bowen conversion in planetary nebulae. Certain discrepancies
between theoretical and observed line ratios are noted, however, which
make the comparison with observation ambiguous. The efficiencies are
shown to be rather insensitive to changes in various parameters. It
is also noted that observations do not necessarily show that the
Bowen lines are systematically weaker in Seyfert galaxy nuclei than
in planetary nebulae.
| Identifer | oai:union.ndltd.org:arizona.edu/oai:arizona.openrepository.com:10150/623859 |
| Date | 01 1900 |
| Creators | Weymann, R. J., Williams, R. E. |
| Contributors | Univ Arizona, Steward Observ |
| Publisher | Steward Observatory, The University of Arizona (Tucson, Arizona) |
| Source Sets | University of Arizona |
| Language | en_US |
| Detected Language | English |
| Type | text, Article |
| Source | Steward Observatory Parker Library SO QB 4 .S752 ARCH |
| Rights | Copyright © All Rights Reserved. |
| Relation | Preprints of the Steward Observatory #17, http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1969ApJ...157.1201W&db_key=AST&data_type=HTML&format=&high=3ed65e9cd005572 |
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