IUE observations of weak G-band stars

Details IUE observations of weak G-band stars IUE observations of weak G-band stars

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984pasp...96...44p&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 96, Jan. 1984, p. 44-53.

Astronomy and Astrophysics

Astronomy

10

Abundance, Giant Stars, Metallicity, Stellar Spectra, Ultraviolet Astronomy, Beryllium, Companion Stars, Emission Spectra, Iue, Lithium, Stellar Luminosity

Scientific paper

High- and low-resolution ultraviolet spectra of several weak G-band giants have been obtained with the IUE satellite, to derive Be abundances and to search for degenerate companions. The abundances of Be in these stars are about log epsilon (Be) approximately -0.5. These values are in good agreement with the Be abundances of Hyades giants, and are consistent with standard theories of post-main-sequence Be depletion in stars. However, the Be abundances do not fit with the large Li abundances in weak G-band stars. Post-main-sequence production of Li or element segregation in main-sequence stars may explain the high Li abundance in weak G-band stars. No direct evidence is seen for the presence of hot subluminous companions. The peculiar abundances in these stars probably are not due to binary mass transfer.

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