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dc.contributor.authorWeymann, R. J.
dc.contributor.authorWilliams, R. E.
dc.date.accessioned2017-06-02T21:26:04Z
dc.date.available2017-06-02T21:26:04Z
dc.date.issued1969-01
dc.identifier.citationAPJ 157: 1201-1213 (Sep. 1969)en
dc.identifier.urihttp://hdl.handle.net/10150/623859
dc.description.abstractThe 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.
dc.language.isoen_USen
dc.publisherSteward Observatory, The University of Arizona (Tucson, Arizona)en
dc.relation.ispartofseriesPreprints of the Steward Observatory #17en
dc.relation.urlhttp://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1969ApJ...157.1201W&db_key=AST&data_type=HTML&format=&high=3ed65e9cd005572en
dc.rightsCopyright © All Rights Reserved.en
dc.sourceSteward Observatory Parker Library SO QB 4 .S752 ARCHen
dc.subjectPlanetary nebulaeen
dc.subjectGalactic nucleien
dc.subjectSeyfert galaxiesen
dc.subjectModelsen
dc.titleThe Bowen Fluorescence Mechanism in Planetary Nebulae and Seyfert Galaxy Nucleien_US
dc.typetexten
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.description.collectioninformationThis title from the Steward Observatory Preprints collection is made available by the Steward Observatory Parker Library and the University Libraries, The University of Arizona. If you have questions about titles in this collection, please contact Parker Library librarian Betty Fridena, bfridena@as.arizona.edu.en
refterms.dateFOA2018-09-11T19:51:22Z
html.description.abstractThe 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.


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