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Shell Stars and Rotationally Unstable Be Stars
Publications of the Astronomical Society of the Pacific, 19631. Shell stars, defined as those having a deep absorption core bordered by emissions in Ha and other lines, arising from transitions between low or metastable levels. We distinguish two types of shell stars: (a) those that have a fairly constant radial velocity, with changes in the total intensity of the emission for example, 28 Tauri; and (b) those ...
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Be Stars as Rotating Stars: Observations
1976The classical rotational hypothesis for Be stars is reviewed and discussed. Methods of measuring rotational velocities are considered and the particular difficulties that Be stars pose in this respect are pointed out. Several tests of the rotational hypothesis are discussed and shown to support this idea. New observations of Balmer emission-line widths
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Astrophysics and Space Science, 2005
A brief review of Be stars in binaries is presented. Attention is paid to systems, where the Be phenomenon is clearly connected to the duplicity, but is not a simple consequence of mass transfer.
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A brief review of Be stars in binaries is presented. Attention is paid to systems, where the Be phenomenon is clearly connected to the duplicity, but is not a simple consequence of mass transfer.
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EAS Publications Series, 2005
Classical Be stars – i.e. non-supergiants B stars with some emission – are very intriguing objects. They represent nearly 20% of B stars. Emission originates in a circumstellar envelope more or less concentrated around the equator, and whose origin is so far unexplained.
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Classical Be stars – i.e. non-supergiants B stars with some emission – are very intriguing objects. They represent nearly 20% of B stars. Emission originates in a circumstellar envelope more or less concentrated around the equator, and whose origin is so far unexplained.
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1969
The Of stars are characterized by broad emission lines of N III 4634, 4641, and He II 4686, in addition to absorption lines shown by normal O-type stars of corresponding spectral type. The presence of these emission features can be understood in terms of selective fluorescence processes proposed by Bowen (1935). Emission can also usually be found at Ha
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The Of stars are characterized by broad emission lines of N III 4634, 4641, and He II 4686, in addition to absorption lines shown by normal O-type stars of corresponding spectral type. The presence of these emission features can be understood in terms of selective fluorescence processes proposed by Bowen (1935). Emission can also usually be found at Ha
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1976
A review of polarization produced in the extended circumstellar disks about Be stars is given. While variability of the polarization and its peculiar wavelength dependence in wide-band continuum measurements are discussed, emphasis is placed upon the recently discovered polarization effects in the emission lines and upon a discussion of models ...
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A review of polarization produced in the extended circumstellar disks about Be stars is given. While variability of the polarization and its peculiar wavelength dependence in wide-band continuum measurements are discussed, emphasis is placed upon the recently discovered polarization effects in the emission lines and upon a discussion of models ...
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