Short-period variability in Be stars

Details Short-period variability in Be stars Short-period variability in Be stars

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.245...92b&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 245, July 1, 1990, p. 92-100.

Astronomy and Astrophysics

Astronomy

100

Angular Velocity, B Stars, Stellar Oscillations, Stellar Rotation, Variable Stars, Astronomical Photometry, Magnetic Field Configurations, Stellar Envelopes, Stellar Magnetic Fields

Scientific paper

A highly significant correlation is found between the projected rotational velocities and the photometric periods of Be stars. It is shown that this correlation may be readily understood if the photometric period is equated with the rotational period. If the nonradial pulsation hypothesis (NRP) is correct, g-modes with radial order exceeding 50 must be involved. According to current NRP theory, these results indicate that the Be stars rotate like solid bodies. On the basis of some recent observations which show that considerable magnetic activity is present and a particular episode in the Be star Kappa CMa, it is suggested that NRP is unlikely to be the cause of low-order periodic variations in Be stars. A model of rotational modulation caused by active areas is proposed.

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