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Paper: Line Profile Variability from Tidal Interactions: Can it Distort the RV Curves?
Volume: 367, Massive Stars in Interactive Binaries
Page: 89
Authors: Koenigsberger, G.; Moreno, E.; Toledano, O.
Abstract: Results of ab initio calculations of the photospheric line-profile variability produced by the tidal interactions in binary systems are presented. A one-layer model is used to compute the effects produced on a primary starís equatorial region by its companion in the general case of arbitrary rotational velocity, eccentricity and viscosity. Radial velocity curves derived from these model computations display small departures from the unperturbed case. The line-profile variability is produced almost entirely by the tangential component of the non-radial pulsation velocity, which can reach values close to the sound speed. This suggests that for massive stars in non-synchronous binary systems the shear produced by the azimuthal motions of the surface layers may lead to localized enhanced activity regions, particularly at the equatorial plane.
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