The dynamical tide in a rotating 10 {M}_\odot main sequence star. A study of g- and r-mode resonances

Details The dynamical tide in a rotating 10 {M}_\odot main sequence star. A study of g- and r-mode resonances The dynamical tide in a rotating 10 {M}_\odot main sequence star. A study of g- and r-mode resonances

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...341..842w&link_type=abstract

Astronomy and Astrophysics, v.341, p.842-852 (1999)

Astronomy and Astrophysics

Astrophysics

24

Stars: Rotation, Stars: Oscillations, Stars: Binaries: Close, Hydrodynamics

Scientific paper

We study the linear, but fully non-adiabatic tidal response of a uniformly rotating, somewhat evolved (Xc=0.4), 10 {M}_\odot main sequence star to the dominant l=2 components of its binary companion's tidal potential. This is done numerically with a 2D implicit finite difference scheme. We assume the spin vector of the 10 {M}_\odot star to be aligned perpendicular to the orbital plane and calculate the frequency bar σ and width of the resonances with the prograde and retrograde gravity (g) modes as well as the resonances with quasi-toroidal rotational (r) modes for varying rotation rates Omega_ {s} of the main sequence star. For all applied forcing frequencies we determine the rate of tidal energy and angular momentum exchange with the companion. In a rotating star tidal energy is transferred from l=2 g-modes to g-modes of higher spherical degree (l=4,6,8,...) by the Coriolis force. These latter modes have shorter wavelength and are damped more heavily, so that the l=2 resonant tidal interaction tends to be reduced for large rotation rates Omega_ {s}. On the other hand, the density of potential resonances (a broad l spectrum) increases. We find several inertially excited unstable l>4 g-modes, but not more than one (retrograde) unstable l=2 g-mode and that only for rapid rotation. Our numerical results can be applied to study the tidal evolution of eccentric binaries containing early type B-star components.

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