All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm]{3425fg1a.ps}\par\includegraphics[angle=-90,width=8.8cm]{3425fg1b.ps}\end{figure}$ Figure 1: Temporal evolution of the eccentricity ( top) and of the inclination ( bottom) of a typical particle trapped in 4:1 resonance with a planet orbiting $\beta\:$ Pic at 10 AU with eccentricity e'=0.07. The planet's mass is 1/1000 of that of the star. The initial eccentricity of the particle is 0.05 and its initial inclination is $2\hbox {$^\circ $ }$ .
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In the text

$\begin{figure} \par\makebox[\textwidth]{ \includegraphics[width=0.49\textwidth]{... ...]{3425fg2c}\hfil \includegraphics[width=0.49\textwidth]{3425fg2d} } \end{figure}$ Figure 2: Level curves of the Hamiltonian $\mathcal{H}$ in the $(\omega ,i)$ plane for the circular problem, for particles having negligible $\sigma$ -libration amplitude, for different values of the constant parameter N. The eccentricity scale (denoted "e'' on the right of the plots) is related to the inclination scale to the left by the constant value of N.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm]{3425fg3a.ps}\par\includegraphics[angle=-90,width=8.8cm]{3425fg3b.ps}\end{figure}$ Figure 3: A statistical test of the inclination oscillation regime for FEBs. These results concern a typical simulation described in Beust & Morbidelli (2000) with e'=0.07 and $\mu =0.002$ . Each dot corresponds to a series of periastron passages of a body that has entered the FEB regime (periastron $\lesssim$ 0.4), and that is not yet fully evaporated. Top plot: inclination as a function of periastron; Bottom plot: inclination as a function of the argument of periastron $\omega$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,origin=br,width=8.8cm]{3425fg4}\end{figure}$ Figure 4: The ab-initio calculated interaction potential between Ca II and H I (in their ground triplet state) as a function of the mutual distance (fat line), superimposed on the induced dipole potential (thin line).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,origin=br,width=8.8cm]{3425fg5}\end{figure}$ Figure 5: The drag force on Ca II ions due to a H I medium of unit density ( $1~\mbox{m}^{-3}$ ), as a function of the drift velocity v. The thin line corresponds to the induced dipole model, the thick grey line to the smooth model (based upon the triplet potential shown in Fig. 4) and the thick black line to the inelastic model (based upon the combination of the triplet potential and a crude treatment for ionization effects, see text).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,origin=br,width=8.8cm]{3425fg6}\end{figure}$ Figure 6: H I column density necessary to stop Ca II ions, as a function of the initial velocity v₀, as derived from Eq. (13), according to several models (see text). The plotting conventions are the same as in Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm]{3425fg1a.ps}\par\includegraphics[angle=-90,width=8.8cm]{3425fg1b.ps}\end{figure}$	Figure 1: Temporal evolution of the eccentricity ( top) and of the inclination ( bottom) of a typical particle trapped in 4:1 resonance with a planet orbiting $\beta\:$ Pic at 10 AU with eccentricity e'=0.07. The planet's mass is 1/1000 of that of the star. The initial eccentricity of the particle is 0.05 and its initial inclination is $2\hbox {$^\circ $ }$ .
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$\begin{figure} \par\makebox[\textwidth]{ \includegraphics[width=0.49\textwidth]{... ...]{3425fg2c}\hfil \includegraphics[width=0.49\textwidth]{3425fg2d} } \end{figure}$	Figure 2: Level curves of the Hamiltonian $\mathcal{H}$ in the $(\omega ,i)$ plane for the circular problem, for particles having negligible $\sigma$ -libration amplitude, for different values of the constant parameter N. The eccentricity scale (denoted "e'' on the right of the plots) is related to the inclination scale to the left by the constant value of N.
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$\begin{figure} \par\includegraphics[angle=-90,origin=br,width=8.8cm]{3425fg4}\end{figure}$	Figure 4: The ab-initio calculated interaction potential between Ca II and H I (in their ground triplet state) as a function of the mutual distance (fat line), superimposed on the induced dipole potential (thin line).
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$\begin{figure} \par\includegraphics[angle=-90,origin=br,width=8.8cm]{3425fg6}\end{figure}$	Figure 6: H I column density necessary to stop Ca II ions, as a function of the initial velocity v₀, as derived from Eq. (13), according to several models (see text). The plotting conventions are the same as in Fig. 5.
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