The Carbon underabundance of the secondary of V356 Sagittarii

Details The Carbon underabundance of the secondary of V356 Sagittarii The Carbon underabundance of the secondary of V356 Sagittarii

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasp..106..365t&link_type=abstract

Publications of the Astronomical Society of the Pacific, vol. 106, no. 698, p. 365-369

Astronomy and Astrophysics

Astronomy

8

Carbon, Eclipsing Binary Stars, Infrared Spectra, Line Spectra, Stellar Composition, Stellar Spectra, Visible Spectrum, Abundance, Iron, Near Infrared Radiation, Nitrogen, Oxygen, Sagittarius Constellation, Stellar Mass Ejection

Scientific paper

We report observations of visual and near-infrared C I, N I, and O I lines in the A2 II secondary of V356 Sagittarii made during a total eclipse of the primary. We confirm the weakness of the secondary's C I lines first seen in ultraviolet observations. Based on a marginal detection of the 9100 A C I lines we estimate that relative to a standard star (HR 7145; AO II) of similar spectral type the (C/Fe) abundance ratio of the secondary is -1.7 plus or minus 0.3 dex. The secondary is not significantly underabundant in N or O. We interpret the C deficiency of the secondary as a result of mass transfer, which has removed its outer layers and exposed its CN-processed interior.

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