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(gzipped) PostScript## The dynamical tide in a rotating main sequence star## A study of g- and r-mode resonances
We study the linear, but fully non-adiabatic tidal response of a
uniformly rotating, somewhat evolved
(),
10 main sequence star to the
dominant 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 star to be aligned
perpendicular to the orbital plane and calculate the frequency
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
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 g-modes to
g-modes of higher spherical degree ()
by the Coriolis force. These latter modes have shorter wavelength and
are damped more heavily, so that the
resonant tidal interaction tends to be reduced for large rotation
rates . On the other hand, the density
of potential resonances (a broad
© European Southern Observatory (ESO) 1999 Online publication: December 16, 1998 |