All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{2538fig1.eps}\end{figure}$ Figure 1: Structure of the heliospheric interface, the region of the interaction of the solar wind and the Local Interstellar Cloud.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2538f2.eps}\end{figure}$ Figure 2: Time variations of the heliocentric distances to the termination shock, bow shock and the heliopause in the upwind direction, and to the termination shock in the downwind direction. Bottom plot shows variations of the solar wind momentum flux, $\rho _E V^2_E$ , with time. Dashed curves correspond to the solution of the problem with the "broken'' first of six solar cycles, when we increased the solar wind ram pressure by factor of 1.5 during the first 11 years of our 66-year periodic calculations.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{2538f3.eps}\end{figure}$ Figure 3: Interstellar plasma number density, velocity, pressure and temperature as functions of the heliocentric distance for two different moments of time: t₁ = 1 year (curves 1), t₂= 6 year (curves 2). Stationary solution (curves 3) and averaged over 11 years time-dependent solution (dots) are shown.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{2538f4.eps}\end{figure}$ Figure 4: Number densities ( top row), bulk velocities ( middle row) and kinetic temperatures ( bottom row) of primary and secondary interstellar atom populations ( left column) and atoms created in the supersonic solar wind and inner heliosheath ( right column) in the upwind direction as functions of the heliocentric distance. Dots, which represent the stationary solution, are practically coincident with solid curves, which represent the 11 year averaged time-dependent solution.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{2538fig5.eps}\end{figure}$ Figure 5: Time-variation of the number densities of primary and secondary interstellar atoms ( top panels), H atoms created in the inner heliosheath and H atoms created in the supersonic solar wind ( bottom panels) as functions of heliocentric distance for two different moments in the solar cycle.
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{2538f6.eps}\end{figure}$ Figure 6: The number densities ( second column from the left), bulk velocities (second column from the right) and kinetic temperatures ( right column) of the primary (solid curves) and secondary (dashed curves) interstellar atom populations and the atoms created in the inner heliosheath (curves with diamonds) at different heliocentric distances in the upwind direction as functions of time. For comparison, the number density of the plasma is shown ( left column). All parameters are non-dimensionlized to their values at t=0.
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,clip]{2538fig7.eps}\end{figure}$ Figure 7: Comparison of variations of density, velocity and kinetic temperature of H atoms created in the inner heliosheath (left column, lines with triangles) with those plasma parameters (right column). The variations are shown at R = 160 AU in the vicinity of the heliopause in the upwind direction for "broken'' solar cycle calculations, where we increase the solar wind ram pressure by factor of 1.5 during the first 11 years of chosen 66-year time-period.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2538fig8.eps}\end{figure}$ Figure 8: Comparison of the time-dependent self-consistent model results (solid curves) with the solution of the time-dependent Euler equation with the source terms (3) taken from the corresponding stationary solution (connected dotted). The figure presents the distribution of plasma number density in the upwind direction for two different moments of the solar cycle. The difference between two models is a few percent.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2538FA0.eps}\end{figure}$ Figure A.1: The sketch of spherical coordinate system. The heliopause and bow shock are shown by the solid lines. The spherical surface approximating the heliopause in the vicinity of the symmetry axis is shown by the dashed line.

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2538bg.eps}\end{figure}$ Figure A.2: The dependences of background quantities in the outer heliosheath on the distance x from the heliopause at the symmetry axis. The upper, middle and lower panels correspond to the density, velocity and temperature. The density is given in $\rho _{\rm p,\infty }$ , the velocity in $v_{\rm p,\infty }$ , and the temperature in 10⁴ K. The distance x from the heliopause is given in AU.

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2538FA1.eps}\end{figure}$ Figure A.3: Evolution of the shape of the wave profile with the distance from the heliopause. $U/\epsilon\hat{u}$ is shown as a function of $\omega \tau = \omega [t - \varphi (x)]$ . The upper, middle and lower panes correspond to x = 0, $x = x_{\rm c} \approx 44.5$ AU, and x = 70 AU. In the lower panel the dashed line shows the unphysical branch of the multivalues function $U(\tau )$ determined by Eq. (A.19). The vertical solid line is the shock.

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2538FA2.eps}\end{figure}$ Figure A.4: The dependence of the velocity jump at the shock on the distance xfrom the heliopause. The velocity is given in km s^-1, and the distance x in AU.

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2538FA3.eps}\end{figure}$ Figure A.5: The snapshots of the wave profile at $\omega t = n\pi$ , $\omega t = (n+1/2)\pi$ and $\omega t = (n+1)\pi$ , where n is any integer number. The dotted vertical lines indicate the bow shock position. The velocity is given in km s^-1 and the distance in AU.

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2538fig1.eps}\end{figure}$	Figure 1: Structure of the heliospheric interface, the region of the interaction of the solar wind and the Local Interstellar Cloud.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{2538f3.eps}\end{figure}$	Figure 3: Interstellar plasma number density, velocity, pressure and temperature as functions of the heliocentric distance for two different moments of time: t₁ = 1 year (curves 1), t₂= 6 year (curves 2). Stationary solution (curves 3) and averaged over 11 years time-dependent solution (dots) are shown.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{2538fig5.eps}\end{figure}$	Figure 5: Time-variation of the number densities of primary and secondary interstellar atoms ( top panels), H atoms created in the inner heliosheath and H atoms created in the supersonic solar wind ( bottom panels) as functions of heliocentric distance for two different moments in the solar cycle.
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