Wave-rotation interaction and episodic mass-loss in Be stars

Details Wave-rotation interaction and episodic mass-loss in Be stars Wave-rotation interaction and episodic mass-loss in Be stars

Jul 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...163...97a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 163, no. 1-2, July 1986, p. 97-104.

Astronomy and Astrophysics

Astrophysics

41

B Stars, Stellar Mass Ejection, Stellar Oscillations, Wave Interaction, Formalism, Nonlinear Equations, Rotary Stability, Stellar Models

Scientific paper

The quasi-periodic oscillation of rotation profile through wave-rotation interaction is shown by linear theory to be possibly in operation in the envelopes of early type stars. The nonlinear behavior of this oscillation is extensively examined for a 20 solar mass ZAMS model, which reveals that it can be amplified in order of magnitude to the phase speed of the waves (nonradial oscillations) and that its time scale (or quasi-period) is inversely proportional to the amount of the pulsational energy of the waves. This oscillation is proposed here as a driving mechanism for the episodic mass-loss of Be stars. It can increase the surface velocity at the equator to the break-up velocity in its acceleration phase. The advantage of this model is that it explains the quasi-periodicity of Be phenomena quite naturally. The observational tests are also discussed based on the predictions by this model. The above model, if it is accepted for Be phenomena, manifests itself as the first example of a stellar cycle related to wave-rotation interaction, the basic idea for which was given by Ando (1982).

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