All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{5776fig1.ps}\end{figure}$ Figure 1: Top: the difference of azimuthal velocity of each surface element and the rigidly rotating inner stellar body, $\Delta V$ ( $\phi$ ) along the equatorial region for a $P_{\rm orb}=$ 5 d binary system. The angle $\phi$ 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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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5776fig2.ps}\end{figure}$ Figure 2: The azimuthal velocity $\Delta V$ ( $\phi$ ) along the equatorial region of surface elements with angle $\phi$ at a given time, for the $P_{\rm orb}=$ 2.5 day binary system and with $\delta R$ = 0.01 R₁ and $\nu =$ 0.0043 $R_\odot ^2$ d^-1.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5776fig3.ps}\end{figure}$ Figure 3: Synchronization timescales (squares) calculated from our tidal oscillation model for a fixed $\beta =$ 2, and $\delta R$ = 0.01 R₁, and for values of $\nu$ as listed in Table 1 compared with Zahn's (1977) relation for stars with convective envelopes (continuous line).
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5776fig4.eps}\end{figure}$ Figure 4: Energy dissipation rates calculated for different viscosities $\nu$ with a fixed layer thickness $\delta R$ = 0.01 R₁ ( left column) and for a changing layer thickness with a fixed viscosity $\nu =$ 0.025 $R_\odot ^2$ d^-1 ( right column). Three binary systems with different orbital periods are illustrated, from top to bottom: $P_{\rm orb}=$ 2.5, 10 and 25 d.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{5776fig5CMJN.eps}\end{figure}$ Figure 5: Energy dissipation rates for different values of $\beta$ , for a binary system with M₁= 5 $M_\odot$ , M₂= 4 $M_\odot$ , R₁= 3.2 $R_\odot$ , $P_{\rm orb}=$ 5 d, $\delta R$ = 0.01 R₁ and $\nu =$ 0.005 $R_\odot ^2$ d^-1.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5776fig2.ps}\end{figure}$	Figure 2: The azimuthal velocity $\Delta V$ ( $\phi$ ) along the equatorial region of surface elements with angle $\phi$ at a given time, for the $P_{\rm orb}=$ 2.5 day binary system and with $\delta R$ = 0.01 R₁ and $\nu =$ 0.0043 $R_\odot ^2$ d^-1.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{5776fig3.ps}\end{figure}$	Figure 3: Synchronization timescales (squares) calculated from our tidal oscillation model for a fixed $\beta =$ 2, and $\delta R$ = 0.01 R₁, and for values of $\nu$ as listed in Table 1 compared with Zahn's (1977) relation for stars with convective envelopes (continuous line).
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$\begin{figure} \par\includegraphics[width=5.8cm,clip]{5776fig4.eps}\end{figure}$	Figure 4: Energy dissipation rates calculated for different viscosities $\nu$ with a fixed layer thickness $\delta R$ = 0.01 R₁ ( left column) and for a changing layer thickness with a fixed viscosity $\nu =$ 0.025 $R_\odot ^2$ d^-1 ( right column). Three binary systems with different orbital periods are illustrated, from top to bottom: $P_{\rm orb}=$ 2.5, 10 and 25 d.
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$\begin{figure} \par\includegraphics[width=7.55cm,clip]{5776fig5CMJN.eps}\end{figure}$	Figure 5: Energy dissipation rates for different values of $\beta$ , for a binary system with M₁= 5 $M_\odot$ , M₂= 4 $M_\odot$ , R₁= 3.2 $R_\odot$ , $P_{\rm orb}=$ 5 d, $\delta R$ = 0.01 R₁ and $\nu =$ 0.005 $R_\odot ^2$ d^-1.
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