There are more absorption line profile-variable Be stars with short periods

Details There are more absorption line profile-variable Be stars with short periods There are more absorption line profile-variable Be stars with short periods

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...134..105b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 134, no. 1, May 1984, p. 105-117.

Astronomy and Astrophysics

Astrophysics

43

Absorption Spectra, B Stars, Stellar Spectra, Variable Stars, Astronomical Photometry, Binary Stars, H Alpha Line, Line Spectra, Radial Velocity

Scientific paper

High resolution, high SNR spectra of the bright Be stars 10 and 28 CMa and HR 4074 suggest that 28 CMa's line profile variability may be a frequent phenomenon among rapidly variable Be stars. Attention is given to examples in which absorption line profile variations are only marginally detected in photographic spectrograms of stars with v sin i of about 200 km/sec, which is the upper limit of the present sample. If the stars in question are close binaries, they are extreme products of the evolution of such systems. Very small total masses, periods and phase angles of line width variations, and the lack of short period eclipsing Be stars, are all noted to be problems for a general binary hypothesis.

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