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The boron abundance of ProcyonThe B I 2496.8 A resonance line and HST/GHRS echelle spectra are used with model atmospheres and synthetic spectra to derive the B abundance of the F dwarfs Procyon (Alpha Canis Minoris), Theta Ursae Majoris, and Iota Pegasi. The B abundance of Theta UMa and Iota Peg is similar to that derived by Boesgaard and Heacox (1978) from the B II resonance line in spectra of A- and B-type stars. These two dwarfs show normal abundances of Li, Be, and B. Procyon, which is highly depleted in Li and Be, is depleted in B by a factor of at least 3. Comparison of the spectra of Procyon and the halo dwarf HD 140283 shows that the B abundance assigned by Duncan et al. (1992) to three halo dwarfs is not greatly overestimated as a result of contamination of the B I line by an unidentified line.
Document ID
19930057067
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Lemke, Michael
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Lambert, David L.
(Texas Univ. Austin, United States)
Edvardsson, Bengt
(Astronomical Observatory Uppsala, Sweden)
Date Acquired
August 16, 2013
Publication Date
May 1, 1993
Publication Information
Publication: Astronomical Society of the Pacific, Publications
Volume: 105
Issue: 687
ISSN: 0004-6280
Subject Category
Astrophysics
Accession Number
93A41064
Funding Number(s)
CONTRACT_GRANT: NAS5-26555
CONTRACT_GRANT: NAG5-1616
Distribution Limits
Public
Copyright
Other

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