All Figures

$\begin{figure} \par\includegraphics[width=11.2cm,clip]{3327fig1.eps} % \par\end{figure}$ Figure 1: The results of the numerical simulation of producing observable comets with galactic disk tide in the absence of any other perturbing forces. The upper part of this figure describes the distribution of the perihelion directions of observable comets on the celestial sphere in the galactic reference frame. The DLDW model of the cloud was used here. The dashed black line denotes the Solar System invariable plane orientation. One cannot observe any concentrations towards this plane - the flattened inner part of the DLDW model does not manifest in the observable population. In the lower part the obtained observable cometary influx versus time is presented.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3327fig2.ps} \end{figure}$ Figure 2: The percentage of the observable part of the cometary cloud "refreshed'' by the stellar passage as a function of the perturber velocity and proximity. The upper panel shows results for the DLDW model and the lower one for the DQT model of the cloud. In both cases, stellar mass equals that of the Sun. Curves a, b, c, d, and e describe results for q_*=10, 30, 50, 70, and 90 thousand of AU, respectively. Note the different vertical scales of these two panels in this figure and the next one.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3327fig3.ps} \end{figure}$ Figure 3: The fraction of the whole cloud removed (i.e. transfered to the "lost'' state, see text) after the stellar passage. The upper panel shows results for the DLDW model and the lower one for the DQT model of the cloud. Again curves a, b, c, d, and e describe the results for the Sun-star minimal distance d_*=10, 30, 50, 70, and 90 thousand of AU, respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3327fig4.ps} \end{figure}$ Figure 4: Dependence of the removed fraction of the whole cloud on the mass and velocity of the stellar perturber. The upper panel shows results for the M_*= 3 $M_{\odot }$ and the lower for M_*= 5 $M_{\odot }$ . Both simulation series were performed for the DLDW model of the cloud. Again curves a, b, c, d, and e describe results for the Sun-star minimal distance q_*=10, 30, 50, 70, and 90 thousand of AU, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=11.2cm,clip]{3327fig5.eps} % % \end{figure}$ Figure 5: Results of the numerical simulation of producing observable comets with stellar impulse and galactic disk tide acting simultaneously. The upper part of this figure describes the distribution of the perihelion directions of observable comets on the celestial sphere in the "stellar'' reference frame. The parameters of the star and its passage are shown in the upper left corner. The dashed black line represents the projection of the star heliocentric orbit plane; star perihelion and anti-perihelion directions are marked with full and empty circles, respectively. The continuous black line denotes the position of the galactic disk plane. In the lower part, the obtained observable cometary influx versus time is presented. To be compared directly with Fig. 7 of Paper I.
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In the text

$\begin{figure} \par\includegraphics[width=11.2cm,clip]{3327fig6.ps} % % \end{figure}$ Figure 6: Results of the numerical simulation of producing observable comets with stellar impulse and galactic disk tide acting simultaneously. In this example the output of the strong stellar perturbation with q_*=30 000 AU is presented. Because of the high efficiency of such an event, we included two additional copies of the directional distribution of perihelion points for two separate time intervals at the bottom of this figure. High concentration of perihelion points in the first 2 mln years is thus clearly visible. Note the characteristic deficiency of perihelion points near the Galactic equator (solid curve in upper part plot). To be compared directly with Fig. 8 of Paper I.
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In the text

$\begin{figure} \par\includegraphics[width=11.2cm,clip]{3327fig7.eps} % % \end{figure}$ Figure 7: The third example the simulation of producing observable comets with stellar impulse and galactic disk tide acting simultaneously, to be compared directly with Fig. 9 of Paper I. It is the case of rather weak (and the most probable) stellar action for q_*= 90 000 AU. The upper plot is presented in the Galactic frame; the straight solid line represents the galactic equator, while the dashed curve represents the heliocentric star orbit plane. In the flux histogram, two consecutive maxima of the same value are clearly shown. The are separated by approx. 9 mln years. A very deep minimum of observable cometary flux occurs 9 mln years after the stellar passage.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3327fig3.ps} \end{figure}$	Figure 3: The fraction of the whole cloud removed (i.e. transfered to the "lost'' state, see text) after the stellar passage. The upper panel shows results for the DLDW model and the lower one for the DQT model of the cloud. Again curves a, b, c, d, and e describe the results for the Sun-star minimal distance d_*=10, 30, 50, 70, and 90 thousand of AU, respectively.
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