All Figures

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{9424f01.eps}\hspace*{4mm} \includegraphics[width=7.7cm,clip]{9424f02.eps}\end{figure}$ Figure 1: Left panel: Kennel & Coroniti total electron energy-distribution function for different values of the maximum particle energy $\epsilon _{\infty }$ as specified in the figure. In the plot, we use $E=\epsilon m c^{2}$ and $F=(f_{{\rm r}}+f_{{\rm w}})\cdot 4{\rm\pi }/(mc^{2})$ and the particle distribution function is normalized to an averaged pressure value of $2.1\times 10^{-9}~{\rm erg~cm^{-3}}$ . The dashed lines are the primordial and the wind component at $\epsilon _{\infty }\rightarrow \infty$ . Right panel: Kennel & Coroniti spectra are plotted against the data. The single contributions from different incident photon targets, thermal FIR emission and total luminosity are reported with different colors and line-styles. Dashed lines: primordial and wind synchrotron contributions and IC-SYN emission; dash-dotted line: thermal FIR and IC-FIR ones; dash-dot-dotted line: IC-CMB one; solid line: total luminosity. References to the observations reported here are given in the main text.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{9424f03.eps}\hspace*{4mm} \includegraphics[width=7.7cm,clip]{9424f04.eps}\end{figure}$ Figure 2: Left panel: runA (1) total electron energy distribution function versus particle energy for different values of maximum particle energy $\epsilon _{{\rm\infty }}$ as specified in the figure. In the plot, we use $E=\epsilon m c^{2}$ and $F=(f_{{\rm r}}+f_{{\rm w}})\cdot 4{\rm\pi }/(mc^{2})$ and the particle distribution function is normalized to an averaged pressure value of $2.1\times 10^{-9}\ {\rm erg~cm^{-3}}$ . The dashed lines are the primordial and the wind component for $\epsilon _{{\rm\infty }}\rightarrow \infty$ . Right panel: runA (1) spectra are plotted against the data. The single contributions from different incident photon targets, thermal FIR emission, and total luminosity are reported with different colors and line-styles. Dashed lines: primordial and wind synchrotron contributions and IC-SYN emission; dash-dotted line: thermal FIR and IC-FIR ones; dash-dot-dotted line: IC-CMB one; solid line: total luminosity. References to the observations reported here are given in the main text.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{9424f05.eps}\hspace*{4mm} \includegraphics[width=7.7cm,clip]{9424f06.eps}\end{figure}$ Figure 3: The same as Fig. 2 for runA (2).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9424f07.eps}\hspace*{4mm} \includegraphics[width=7.3cm,clip]{9424f08.eps}\end{figure}$ Figure 4: Left panel: color-coded map of the thermal pressure in units of ${\rm erg~cm}^{-3}$ . Right panel: color-coded map of the maximum particle energy; superimposed contours correspond to values of 10⁷ (solid line), 10⁸ (dotted line), 10⁹ (dashed line), and 10¹⁰ (dot-dashed line). Along the axes, distance from the central pulsar is reported in ly.
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,height=6cm,clip]{9424f09.eps}\hs... ...ace*{4mm} \includegraphics[width=5.2cm,height=6cm,clip]{9424f11.eps}\end{figure}$ Figure 5: RunA (2) case. Simulated total surface-brightness maps in logarithmic scale normalized to the maximum at different IC frequency cut-offs: on the left at 4 GeV with a maximum $\approx$ 1.6 $\times 10^{-28}$ ${\rm erg}$ ${\rm cm^{-2}~sr^{-1}~s^{-1}~Hz^{-1}}$ ; in the middle at 250 GeV with a maximum $\approx$ 1.0 $\times 10^{-29}$ ${\rm erg}$ ${\rm cm^{-2}~sr^{-1}~s^{-1}~Hz^{-1}}$ ; on the right at 1 TeV with a maximum $\approx$ 1.8 $\times 10^{-30}$ ${\rm erg}$ ${\rm cm^{-2}~sr^{-1}~s^{-1}~Hz^{-1}}$ . On the axes: distance from the central pulsar in unit of ly.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{9424f12.eps}\end{figure}$ Figure 6: RunA (2) case. Snapshots from a movie of PWN evolution: output times are selected at 950.6 yr, 955.4 yr, and 960.0 yr. Results from one output time per row are shown. Left panels: plot of the synthetic spectral luminosity in logarithmic scale versus photon frequencies (log). Middle panels: simulated brightness maps (log) at 1 keV normalized to the maximum $6.2\times 10^{-18}~{\rm erg}~{\rm cm^{-2}~sr^{-1}~s^{-1}~Hz^{-1}}$ . Right panels: simulated brightness maps (log) at 250 GeV normalized to the maximum $1.2\times 10^{-29}~{\rm erg}~{\rm cm^{-2}~sr^{-1}~s^{-1}~Hz^{-1}}$ . The x and y axes of all surface brightness maps report the distance (in ly) from the central pulsar. We indicate the inclination with respect to both the plane of the sky and the north direction: respectively $30^{\circ }$ and $48^{\circ }$ for the Crab Nebula. We note that only the internal region (within a radius of 3 ly) is displayed.
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In the text

$\begin{figure} \par\includegraphics*[bb=0 -10 509 368,width=7.5cm,clip]{9424f13.eps}\end{figure}$ Figure 7: RunA (2) case. Total luminosity $\nu L_\nu$ in unit 10³⁴ erg ${\rm s^{-1}}$ s is displayed as a function of time, from t = 950 yr to t = 960 yr. From top to bottom panels, the corresponding photon energies are 1 keV, 40 MeV, 1 TeV.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{9424f05.eps}\hspace*{4mm} \includegraphics[width=7.7cm,clip]{9424f06.eps}\end{figure}$	Figure 3: The same as Fig. 2 for runA (2).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9424f07.eps}\hspace*{4mm} \includegraphics[width=7.3cm,clip]{9424f08.eps}\end{figure}$	Figure 4: Left panel: color-coded map of the thermal pressure in units of ${\rm erg~cm}^{-3}$ . Right panel: color-coded map of the maximum particle energy; superimposed contours correspond to values of 10⁷ (solid line), 10⁸ (dotted line), 10⁹ (dashed line), and 10¹⁰ (dot-dashed line). Along the axes, distance from the central pulsar is reported in ly.
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$\begin{figure} \par\includegraphics*[bb=0 -10 509 368,width=7.5cm,clip]{9424f13.eps}\end{figure}$	Figure 7: RunA (2) case. Total luminosity $\nu L_\nu$ in unit 10³⁴ erg ${\rm s^{-1}}$ s is displayed as a function of time, from t = 950 yr to t = 960 yr. From top to bottom panels, the corresponding photon energies are 1 keV, 40 MeV, 1 TeV.
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