Figure 1: Top: the difference of azimuthal velocity of each surface element and the rigidly rotating inner stellar body, () along the equatorial region for a 5 d binary system. The angle is measured with respect to the line connecting the two stars. Bottom: the component of the velocity in the radial direction of each surface element along the equatorial belt for the same model. The star is rotating at twice the orbital frequency. | |
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Figure 2: The azimuthal velocity () along the equatorial region of surface elements with angle at a given time, for the 2.5 day binary system and with = 0.01 R_{1} and 0.0043 d^{-1}. | |
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Figure 3: Synchronization timescales (squares) calculated from our tidal oscillation model for a fixed 2, and = 0.01 R_{1}, and for values of as listed in Table 1 compared with Zahn's (1977) relation for stars with convective envelopes (continuous line). | |
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Figure 4: Energy dissipation rates calculated for different viscosities with a fixed layer thickness = 0.01 R_{1} ( left column) and for a changing layer thickness with a fixed viscosity 0.025 d^{-1} ( right column). Three binary systems with different orbital periods are illustrated, from top to bottom: 2.5, 10 and 25 d. | |
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Figure 5: Energy dissipation rates for different values of , for a binary system with M_{1}= 5 , M_{2}= 4 , R_{1}= 3.2 , 5 d, = 0.01 R_{1} and 0.005 d^{-1}. | |
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