All Figures

$\begin{figure} \par\mbox{\includegraphics[width=8cm]{4089fi1a.ps} \includegraphi... ...idth=8cm]{4089fi1e.ps} \includegraphics[width=8cm]{4089fi1f.ps} } \end{figure}$ Figure 1: Comparison of temperature ( top), density ( middle), and ionization fraction ( bottom) plots of the old model i ( left) and model i $^\prime$ ( right) at day 74. Besides slight differences in the internal morphology, the dimensions of the jets, positions of the internal shocks, and temperatures are identical in both simulations; differences in the ionization fractions arise in the low-temperature regions of the jet due to the larger equilibration timescales in this temperature range.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8cm]{4089fi2a.ps} \includegraphi... ...idth=8cm]{4089fi2g.ps} \includegraphics[width=8cm]{4089fi2h.ps} } \end{figure}$ Figure 2: $\rho - T$ -histogram of eight consecutive days (day 62-69) covering one pulse cycle of model i ( left) and model i $^\prime$ ( right). The bright bar at very low temperatures and at densities between 10^-16 and 10^-14 g cm^-3 consists of the external medium. The internal dense knots build up the line at T = 10⁴ K. The new pulse becomes visible as an arc and spreads out along a line of constant temperature.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8cm]{4089fi3a.ps} \includegraphi... ...idth=8cm]{4089fi3g.ps} \includegraphics[width=8cm]{4089fi3h.ps} } \end{figure}$ Figure 3: As Fig. 2, continued. The radiative cooling lowers the temperature of the region of higher densities. Superposed on it, the whole feature moves towards lower densities and lower temperatures, consistent with adiabatic expansion. The slope of the path is approximately $\log ( T ) \sim 2 / 3 ~ \log ( \rho )$ .
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{4089fig4.eps}} \end{figure}$ Figure 4: Size of the bow-shock in axial and radial direction for model i $^\prime$ . After a phase of constant radial extent and therefore acceleration of the axial bow-shock, the jet head grows, leading to a constant propagation velocity of the jet.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{4089fig5.eps}} \end{figure}$ Figure 5: Slices of density along the jet axis for model i $^\prime$ at days 30, 40, 50, 60, and 70, respectively. The last four lines are shifted downwards by 3, 6, 9, and 12 orders of magnitude, respectively, for clarity. After day 70, the density of the first internal shock behind the bow-shock is larger than the density of the surrounding medium, which then leads to the substantial change in kinematics.
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In the text

$\begin{figure} \mbox{\includegraphics[width=8cm]{4089fi6a.ps} \includegraphics[... ...idth=8cm]{4089fi6e.ps} \includegraphics[width=8cm]{4089fi6f.ps} } \end{figure}$ Figure 6: Logarithm of density for model i $^\prime$ on day 162 and for model iv $^\prime$ on day 115. The extent of the knots in the jet beam is enlarged with respect to the former model i with cooling. No cocoon and no backflow are present; in model iv $^\prime$ the internal structure is more complicated than in model i $^\prime$ and the knots are drifting away from the jet axis.
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In the text

$\begin{figure} \mbox{ \includegraphics[width=8cm]{4089fi7a.ps} \includegraphics... ...idth=8cm]{4089fi7k.ps} \includegraphics[width=8cm]{4089fi7l.ps} } \end{figure}$ Figure 7: Radiative properties of model i $^\prime$ on day 162 ( left) and model iv $^\prime$ on day 115 ( right): the emissivity of bremsstrahlung and optical emission in erg s^-1 cm^-3, emission maps of bremsstrahlung and optical emission in erg s^-1 cm^-2 with an assumed distance of 200 pc - with and without a detection threshold of 10^-15 erg s^-1 cm^-2. The emission of the internal knots is blended by the emission of the dense radiative shell of shocked ambient medium.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4089fig8.eps}} \end{figure}$ Figure 8: Sequence of absorption line profiles for eight consecutive days for model i $^\prime$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4089fig9.eps}} \end{figure}$ Figure 9: Sequence of absorption line profiles for eight consecutive days of model iv $^\prime$ .
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8cm]{4089fi3a.ps} \includegraphi... ...idth=8cm]{4089fi3g.ps} \includegraphics[width=8cm]{4089fi3h.ps} } \end{figure}$	Figure 3: As Fig. 2, continued. The radiative cooling lowers the temperature of the region of higher densities. Superposed on it, the whole feature moves towards lower densities and lower temperatures, consistent with adiabatic expansion. The slope of the path is approximately $\log ( T ) \sim 2 / 3 ~ \log ( \rho )$ .
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$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{4089fig4.eps}} \end{figure}$	Figure 4: Size of the bow-shock in axial and radial direction for model i $^\prime$ . After a phase of constant radial extent and therefore acceleration of the axial bow-shock, the jet head grows, leading to a constant propagation velocity of the jet.
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$\begin{figure} \mbox{\includegraphics[width=8cm]{4089fi6a.ps} \includegraphics[... ...idth=8cm]{4089fi6e.ps} \includegraphics[width=8cm]{4089fi6f.ps} } \end{figure}$	Figure 6: Logarithm of density for model i $^\prime$ on day 162 and for model iv $^\prime$ on day 115. The extent of the knots in the jet beam is enlarged with respect to the former model i with cooling. No cocoon and no backflow are present; in model iv $^\prime$ the internal structure is more complicated than in model i $^\prime$ and the knots are drifting away from the jet axis.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4089fig8.eps}} \end{figure}$	Figure 8: Sequence of absorption line profiles for eight consecutive days for model i $^\prime$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4089fig9.eps}} \end{figure}$	Figure 9: Sequence of absorption line profiles for eight consecutive days of model iv $^\prime$ .
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