An unusually short stable period of absorption line asymmetries and V/R variations in the spectrum of the Be star 28 CMa

Details An unusually short stable period of absorption line asymmetries and V/R variations in the spectrum of the Be star 28 CMa An unusually short stable period of absorption line asymmetries and V/R variations in the spectrum of the Be star 28 CMa

Jan 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...105...65b&link_type=abstract

Astronomy and Astrophysics, vol. 105, no. 1, Jan. 1982, p. 65-75.

Astronomy and Astrophysics

Astrophysics

91

Absorption Spectra, B Stars, Early Stars, Periodic Variations, Radial Velocity, Stellar Spectra, Variable Stars, Asymmetry, Emission Spectra, Stellar Spectrophotometry

Scientific paper

In 28 CMa (B2-3, IV-Ve, mV ≃ 3m.8) the by far shortest stable period known of Be stars has been detected. The 1 .365-d periodicity affects the profiles of absorption lines (changing asymmetry), the radial velocities of emission lines and their V/R ratios. The radial velocity curves obtained from measurements of the absorption line minima (maximum transparency) can be arranged in several groups according to their amplitudes. Between different groups no phase shifts occur while absorption and emission lines differ in phase by almost exactly 180 degrees. The short period, the changing asymmetry of line profiles, and the absence of pronounced photometric variability (Δm ≤= 0m.03 in uvby) related to the spectroscopic period, greatly impede the application of existing models for Be stars to 28 CMa. Because of numerous similarities to β Cephei stars, an attempt has been made to develop a model of nonradial pulsations for 28 CMa. It is shown that P22-pulsations can explain not only all of the observed spectroscopic variations of 28 CMa, but also because of the assumed retrograde motion of the travelling waves, the much more frequently observed long "period" V/R variations of other Be stars.

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