Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=17cm,clip]{0258fig1.eps} \end{figure}$ Figure 1: a) The time scales for spiralling into the host stars (according to Eq. (5)) of the extrasolar planets located at semi major axis of today. The symbols mark the average value of $\frac{Q_*}{k_{2*}}$ , the error bar the selected range of $\frac{Q_*}{k_{2*}}$ (see Sect. 2). b) The Doodson constant of extrasolar planets with e=0 for a semi major axis less than 0.06 AU.
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In the text

$\begin{figure} \par\includegraphics[width=17.3cm,clip]{0258fig2.eps} \end{figure}$ Figure 2: The change in semi major axis of OGLE-TR-56 b a) and OGLE-TR-3 b b) within 5 billion years for different values $\frac{Q_*}{k_{2*}}$ . For values of $\frac{Q_*}{k_{2*}}$ smaller than the average, the planet needs less than a few billion years to spiral into the star.
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In the text

$\begin{figure} \par\includegraphics[width=17.1cm,clip]{0258fig3.eps} \end{figure}$ Figure 3: The change in stellar rotation period of the host stars of OGLE-TR-56 b a) and OGLE-TR-3 b b) due to tidal friction.In this case, it was assumed that the stellar body is rigid. For values of $\frac{Q_*}{k_{2*}}$ smaller than the average, the star is significantly spun up.
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In the text

$\begin{figure} \par\includegraphics[width=17.3cm,clip]{0258fig4.eps} \end{figure}$ Figure 4: The change in stellar rotation period of the host stars of OGLE-TR-56 b a) and OGLE-TR-3 b b) due to tidal friction. In this case, it was assumed that the tidal enery is dissipated in the outer stellar layers. Neglecting friction between the outer layers and the core, the spin-up of the outer stellar layer is significant even for the maximum value of $\frac{Q_*}{k_{2*}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0258fig1.eps} \end{figure}$	Figure 1: a) The time scales for spiralling into the host stars (according to Eq. (5)) of the extrasolar planets located at semi major axis of today. The symbols mark the average value of $\frac{Q_}{k_{2}}$ , the error bar the selected range of $\frac{Q_}{k_{2}}$ (see Sect. 2). b) The Doodson constant of extrasolar planets with e=0 for a semi major axis less than 0.06 AU.
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$\begin{figure} \par\includegraphics[width=17.3cm,clip]{0258fig2.eps} \end{figure}$	Figure 2: The change in semi major axis of OGLE-TR-56 b a) and OGLE-TR-3 b b) within 5 billion years for different values $\frac{Q_}{k_{2}}$ . For values of $\frac{Q_}{k_{2}}$ smaller than the average, the planet needs less than a few billion years to spiral into the star.
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$\begin{figure} \par\includegraphics[width=17.1cm,clip]{0258fig3.eps} \end{figure}$	Figure 3: The change in stellar rotation period of the host stars of OGLE-TR-56 b a) and OGLE-TR-3 b b) due to tidal friction.In this case, it was assumed that the stellar body is rigid. For values of $\frac{Q_}{k_{2}}$ smaller than the average, the star is significantly spun up.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=17.3cm,clip]{0258fig4.eps} \end{figure}$	Figure 4: The change in stellar rotation period of the host stars of OGLE-TR-56 b a) and OGLE-TR-3 b b) due to tidal friction. In this case, it was assumed that the tidal enery is dissipated in the outer stellar layers. Neglecting friction between the outer layers and the core, the spin-up of the outer stellar layer is significant even for the maximum value of $\frac{Q_}{k_{2}}$ .
Open with DEXTER