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On the ultraviolet iron spectrum of pre-white dwarfsNumerous lines of Fe V, Fe VI, and Fe VII have been detected in high-resolution IUE spectra of two central stars and a number of very hot subdwarfs. The strengths of these lines vary widely from star to star, suggesting that the abundance of iron in the atmospheres of the immediate progenitors of white dwarfs is strongly variable. A possible explanation is elemental separation by gravity and radiation pressure.
Document ID
19850048766
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
doi:10.1086/184440
Authors
Schoenberner, D. (Kiel, Universitaet Institut fuer theoretische Physik und Sternwarte, Kiel, Germany)
Drilling, J. S. (Louisiana State University Baton Rouge, LA, United States)
Date Acquired
August 12, 2013
Publication Date
March 15, 1985
Publication Information
Publication: Astrophysical Journal, Part 2 - Letters to the Editor
Volume: 290
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
85A30917
Funding Number(s)
CONTRACT_GRANT: NSF AST-80-18766
CONTRACT_GRANT: NAG5-71
CONTRACT_GRANT: NSF INT-82-19240
Distribution Limits
Public
Copyright
Other

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