Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2946fig1.eps}\end{figure}$ Figure 1: For illustration of the Roche potentials we calculate the potentials for a planetary system with a mass ratio of 0.013 a) in three dimensions and b) as contours. The square in b) is blown up in c). The two peaks in a) show the potential close to the star and planet, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.35cm,clip]{2946fig2.eps}\end{figure}$ Figure 2: Relevant radii $r_{\rm X=1.5}$ and $r_{\rm L1}$ for OGLE-TR-56 b, OGLE-TR-10 b, OGLE-TR-111 b and HD 209458 b. For OGLE-TR-56 b, $r_{\rm L1}$ is clearly less than $r_{\rm X=1.5}$ , which indicates that the exoplanet is most likely in a stage of geometric blow-off, while the three other exoplanets are most likely in a stage of a classical hydrodynamic blow-off regime.
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In the text

$\begin{figure} \par\includegraphics[height=3.8cm,width=7.65cm,clip]{2946fig3.eps}\end{figure}$ Figure 3: Left panel: expanded atmosphere of HD 209458 b under the influence of the tidal forces of its host star, which is pictured as a point-mass. The size of the planet is not in scale. Right panel: detailed view of the normalized expanded atmosphere of HD 209458 b under the influence of tidal forces. Note that the tidal deformation leads to an atmospheric radius which slightly deviates form the more idealized expansion radius $r_{\rm exp}$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2946fig1.eps}\end{figure}$	Figure 1: For illustration of the Roche potentials we calculate the potentials for a planetary system with a mass ratio of 0.013 a) in three dimensions and b) as contours. The square in b) is blown up in c). The two peaks in a) show the potential close to the star and planet, respectively.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.35cm,clip]{2946fig2.eps}\end{figure}$	Figure 2: Relevant radii $r_{\rm X=1.5}$ and $r_{\rm L1}$ for OGLE-TR-56 b, OGLE-TR-10 b, OGLE-TR-111 b and HD 209458 b. For OGLE-TR-56 b, $r_{\rm L1}$ is clearly less than $r_{\rm X=1.5}$ , which indicates that the exoplanet is most likely in a stage of geometric blow-off, while the three other exoplanets are most likely in a stage of a classical hydrodynamic blow-off regime.
Open with DEXTER