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$\begin{figure} \par\includegraphics[width=4.8cm,clip]{4774f1.eps} \end{figure}$ Figure 1: A schematic view of a dust aggregate irradiated by stellar wind ions. The shadow on the xy plane expresses the geometrical cross section of the aggregate.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{4774f2a.eps}\includegraphics[width=6cm,clip]{4774f2b.eps} \end{figure}$ Figure 2: Models of dust aggregates.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{4774f3a.eps}\hspace*{4mm}\includegraphics[width=5.8cm,clip]{4774f3b.eps} \end{figure}$ Figure 3: Momentum transfer cross section averaged over aggregate orientations, $\bar C_{\rm sw}$ , for ballistic cluster-cluster aggregates (BCCAs; left) and ballistic particle-cluster aggregates (BPCAs; right) versus the number of monomers N. The vertical axis shows $\bar C_{\rm sw}$ divided by the geometrical cross section of a sphere of the same volume as the aggregate. The lines indicate the cross section given by the empirical formula Eq. (15). In the figure, $a_{\rm v}=N^{1/3}a$ is the radius of volume-equivalent spheres and X=2a/l(p₀) is the size parameter of monomers, where a is the monomer radius and l(p₀) is the projected range of stellar wind ions.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{4774f4a.eps}\hspace*{4mm}\in... ...4c.eps}\hspace*{4mm}\includegraphics[width=5.8cm,clip]{4774f4d.eps} \end{figure}$ Figure 4: The ratio $\beta _{\rm sw}$ of the solar wind pressure to gravitational attraction by the sun for aggregates: a) silicate BCCAs (ballistic cluster-cluster aggregates), b) silicate BPCAs (ballistic particle-cluster aggregates), c) carbon BCCAs, d) carbon BPCAs. The solid and dashed curves are the $\beta _{\rm sw}$ ratios with the monomer radius of 0.1 and 0.01 $\mu$ m, respectively. The dotted line indicates the ratio $\beta _{\rm sw}$ for a spherical dust taking into account the effect of passage of incident ions through the dust grains. Here, $a_{\rm v}$ is the radius of volume-equivalent spheres.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{4774f5a.eps}\hspace*{4mm}\includegraphics[width=6cm,clip]{4774f5b.eps} \end{figure}$ Figure 5: Ratio $\gamma$ of the plasma PR drag to the photon PR drag for silicate and carbon aggregates consisting of 0.1 $\mu$ m-radius monomers. The right axis indicates the ratio of the stellar wind pressure to the radiation pressure. Solid, dash-dotted, and dotted lines are the results for ballistic particle-cluster aggregates (BPCAs), ballistic cluster-cluster aggregates (BCCAs), and spheres, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{4774f6a.eps}\hspace*{4mm}\includegraphics[width=5.8cm,clip]{4774f6b.eps} \end{figure}$ Figure 6: Falling time for ballistic particle-cluster aggregates (BPCAs; solid lines) and ballistic cluster-cluster aggregates (BCCA; dash-dotted lines) and for spherical particles (dotted lines) from 50 AU from a central star. The left and right axes indicate the falling times for the mass loss rates of 1 and $100~\dot M_{\odot}$ , respectively. The dashed line is the falling time for spherical particles due to the photon PR effect under the solar luminosity of $1~L_{\odot}$ (see the left axis). Note that the range of luminosities of young main-sequence stars is limited around $\sim$ $1~L_{\odot}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4774fa1.eps} \end{figure}$ Figure A.1: Geometrical cross sections of aggregates, $\bar S_z$ , relative to the sum of monomer cross sections, $N\pi a^2$ . Mean values are plotted by symbols, their standard deviations are given by error bars, and fitting curves are indicated by dotted lines. Squares: ballistic cluster-cluster aggregates (BCCAs); Circles: ballistic particle-cluster aggregates (BPCAs).

In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{4774fb1.eps} \end{figure}$ Figure B.1: Dust-removal processes in the phase space for the mass loss rate of a star $\dot M$ and the total dust mass of its circumstellar disk $M_{\rm d}$ . The dominant process is determined by the shortest lifetime among Eqs. (B.1)-(B.3).

In the text

$\begin{figure} \par\includegraphics[width=4.8cm,clip]{4774f1.eps} \end{figure}$	Figure 1: A schematic view of a dust aggregate irradiated by stellar wind ions. The shadow on the xy plane expresses the geometrical cross section of the aggregate.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{4774f2a.eps}\includegraphics[width=6cm,clip]{4774f2b.eps} \end{figure}$	Figure 2: Models of dust aggregates.
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