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The Bowen Fluorescence Mechanism in Planetary Nebulae and Seyfert Galaxy Nuclei

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.

Identiferoai:union.ndltd.org:arizona.edu/oai:arizona.openrepository.com:10150/623859
Date01 1900
CreatorsWeymann, R. J., Williams, R. E.
ContributorsUniv Arizona, Steward Observ
PublisherSteward Observatory, The University of Arizona (Tucson, Arizona)
Source SetsUniversity of Arizona
Languageen_US
Detected LanguageEnglish
Typetext, Article
SourceSteward Observatory Parker Library SO QB 4 .S752 ARCH
RightsCopyright © All Rights Reserved.
RelationPreprints 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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