Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...417..697l&link_type=abstract
Astrophysical Journal v.417, p.697
Astronomy and Astrophysics
Astronomy
8
Stars: Binaries: Close, Stars: Early-Type, Stars: Interiors, Stars: Oscillations
Scientific paper
We discuss angular momentum transfer by tidally forced oscillations (the dynamical tides) in a massive main-sequence star in a binary system. Because of the periodic gravitational disturbance by the orbital motion of the companion star, low-frequency global oscillations are excited as dynamical tides in the massive mainsequence star. We are mainly interested in the case where the orbital motion of the companion star is in resonance with low-order quadrupole g-modes of the main-sequence star. Dissipation mechanisms associated with nonaxisymmetric oscillations are known to play essential roles in angular momentum transfer in stars. We show that the deep interior of a massive main-sequence star is a damping (positively dissipative) region and the outer envelope is an excitation (negatively dissipative) region for low-order g-modes. We also show that the tidally forced oscillations whose frequency range overlaps with that of the g-modes have almost the same dissipative (nonadiabatic) properties as the g-modes. It is shown that the rotation of the outer envelope of a massive main-sequence star is driven, by the tidally forced oscillations, in the opposite direction to the orbital motion, as observed in the corotating frame of the main-sequence star. We show that forcing on the outer envelope by a tidal oscillation can be strong enough when the tidal oscillation is in resonance with one of the low-order g-modes of the star. We suggest that tidal oscillations could supply enough angular momentum to support an excretion disk around a Be star (a rapidly rotating massive main-sequence star) in a high mass X-ray binary system.
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