Observations of the mid-ultraviolet spectrum of peculiar A and B stars and of Be stars, BN stars and shell stars

Details Observations of the mid-ultraviolet spectrum of peculiar A and B stars and of Be stars, BN stars and shell stars Observations of the mid-ultraviolet spectrum of peculiar A and B stars and of Be stars, BN stars and shell stars

Feb 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....82...48l&link_type=abstract

Astronomy and Astrophysics, vol. 82, no. 1-2, Feb. 1980, p. 48-52.

Astronomy and Astrophysics

Astrophysics

5

A Stars, B Stars, Early Stars, Shell Stars, Stellar Spectra, Stellar Structure, Ultraviolet Spectra, Abundance, Emission Spectra, Line Spectra, Stellar Luminosity

Scientific paper

The mid ultraviolet spectrum of bright early type stars of spectral types Ap, Bp, Be, Bn, and shell stars is studied. The intrinsic color at 2500 Å, (m2500 - V)0, and the strength of the Fe II feature at 2548 Å and of the Fe III feature at 2078 Å are compared with those of normal stars. Six out of the nine peculiar A and B stars are flux deficient in (m2500 - V)0 and eight out of the nine have a too strong Fe II feature and usually a too weak Mg II feature. Most of the Be stars have a normal (m2500 - V)0 color and a too weak Fe II feature which might even be in emission in the hottest ones. The Fe Ill feature and the Mg II feature are too weak in most Be stars. The color (m2500 - V)0 of the binary β Lyr indicates a luminosity class II, in agreement with the hydrogen lines.

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