Other
Scientific paper
Jul 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1761b&link_type=abstract
IUE Proposal ID #AFGEB
Other
Scientific paper
Lambda Boo stars show abnormally weak metallic lines for their spectral type, if this is determined from the ratio of the CaII K to hydrogen line strength, yet they are no population II stars as shown by their low space velocities and by their apparently large rotational velocities which are around 100 km/sec. (Baschek and Searle,.1969). Spectrum analysis shows a metal deficiency except that OI has normal abundances and CI seems to be actually overabundant (Saschek et al 1983). The UV spectra suggest that another light source is contributing to the continuous light. It appears that the strong CI lines seen in the Lambda Boo uv spectrum may be formed in a shell of carbon rich material. We want to observe additional lambda Boo stars in order to see whether this interpretation fits all lambda Boo stars. We would like to re-observe lambda Boo in order to see whether time variations in the CI lines can be observed, which would support the interpretation as envelope lines. We want to study in detail the binary ADS 3910 which contains one A Boo star and one apparently normal B8V star (Sargent, 1966).
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