All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip,bb= 44 93 503 397,clip]{1219fig1.eps} \end{figure}$ Figure 1: The mean value of the 1/r⁶ term of the tidal torque, compared to $1/r_{\rm sr}^6$ , where $r_{\rm sr}$ is the semilatus rectum. Except for very large eccentricities, $1/r_{\rm sr}^6$ is an acceptable approximation of $\langle 1/r^6\rangle$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip, bb= 51 86 494 404]{1219fig2.eps} \end{figure}$ Figure 2: Distribution of the SB in the ( $P_{\rm sr}$ - e) diagram, where $P_{\rm sr}$ is the period that the SB would have if their orbits became circular with the same angular momenta. The symbols represent the systems with different mass ratios. The code is as follows: $q \leq 0.4$ , circles; $0.4 < q \leq 0.8$ , squares; $q \leq 0.8$ (maximum q for SB1) and minimum $q \leq 0.4$ , small diamonds; q > 0.8 (twins), open triangles. The thin dotted line is the limit $e_{\rm Sup}$ corresponding to a maximum period of 10 years, as derived from Eq. (2).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip, bb= 50 86 495 404]{1219fig3.eps} \end{figure}$ Figure 3: Distribution of the SB in the period-eccentricity diagram. The symbols are the same as in Fig. 2. The lines refer to the median eccentricities of the different classes of mass ratios : $q \leq 0.4$ , thick full line; $0.4 < q \leq 0.8$ , thick dashes; all $q \leq 0.8$ , thick dot-dashed line; q > 0.8 (twins), thin line. The 2 thin dotted lines are the limits of the location of SB with $P_{\rm sr}$ between 5 and 10 days, as derived from Eq. (3).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip, bb= 50 86 495 404]{1219fig4.eps} \end{figure}$ Figure 4: Same as Fig. 2 for the planets. The circles are the planets with minimum mass <2 Jupiter, and the open squares refer to the others. The thin dotted line is the limit $e_{\rm Sup}$ corresponding to a maximum period of 2200 days.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip, bb= 50 86 494 404]{1219fig5.eps} \end{figure}$ Figure 5: Same as Fig. 3 for the exoplanets. The symbols are the same as in Fig. 4. The full line is the median eccentricity of the planets with minimum mass <2 Jupiter, and the dashes refer to the masses heavier than 2 Jupiter. The thin dotted line is the eccentricity $e_{\rm Max}$ corresponding to a circularized period of 5 days.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip, bb= 51 86 495 404]{1219fig6.eps} \end{figure}$ Figure 6: The exoplanets compared to the non-twin binaries in the(P - e) diagram. The circles refer to the planets, and the open squares to the SB with $q \leq 0.8$ . The thin dotted line is $e_{\rm Max}$ , the maximum eccentricity when the circularization limit is $P_{\rm cutoff}=10$ days. The median eccentricities are derived after discarding the systems above this limit, in order to have the same selection effects for both samples. The median eccentricity of the planets is given by a full line, and that of the SB by a a dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip, bb= 54 93 504 404]{1219fig7.eps} \end{figure}$ Figure 7: Distribution of the eccentricities of SB and planets corrected for tidal circularization.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip,bb= 44 93 503 397,clip]{1219fig1.eps} \end{figure}$	Figure 1: The mean value of the 1/r⁶ term of the tidal torque, compared to $1/r_{\rm sr}^6$ , where $r_{\rm sr}$ is the semilatus rectum. Except for very large eccentricities, $1/r_{\rm sr}^6$ is an acceptable approximation of $\langle 1/r^6\rangle$ .
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$\begin{figure} \par\includegraphics[width=8.2cm,clip, bb= 50 86 495 404]{1219fig4.eps} \end{figure}$	Figure 4: Same as Fig. 2 for the planets. The circles are the planets with minimum mass <2 Jupiter, and the open squares refer to the others. The thin dotted line is the limit $e_{\rm Sup}$ corresponding to a maximum period of 2200 days.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip, bb= 50 86 494 404]{1219fig5.eps} \end{figure}$	Figure 5: Same as Fig. 3 for the exoplanets. The symbols are the same as in Fig. 4. The full line is the median eccentricity of the planets with minimum mass <2 Jupiter, and the dashes refer to the masses heavier than 2 Jupiter. The thin dotted line is the eccentricity $e_{\rm Max}$ corresponding to a circularized period of 5 days.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip, bb= 54 93 504 404]{1219fig7.eps} \end{figure}$	Figure 7: Distribution of the eccentricities of SB and planets corrected for tidal circularization.
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