Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1794fig1.eps} \end{figure}$ Figure 1: Spectrum of protons released from a source at R=10 pc after t=100 yr (solid line) and 10 000 yr (long-dashed line). The dotted horizontal line shows the flux of cosmic ray protons observed near the Earth. a) For an impulsive MQ. b) For a continuous MQ.
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In the text

$\begin{figure} \includegraphics[width=8.6cm,clip]{1794fig2.eps} \end{figure}$ Figure 2: Proton and electron energy distributions (solid and long-dashed lines respectively) for an impulsive MQ at R=10 pc. The kinetic energy axis units are m $_{\rm e}$ c². a) The source age is t=100 yr. b) The source age is 1000 yr.
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In the text

$\begin{figure} \includegraphics[width=8.6cm,clip]{1794fig3.eps} \end{figure}$ Figure 3: The same as in Fig. 2 but for a continuous MQ (recall: a) t=100 yr; b) t=1000 yr).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1794fig4.eps} \end{figure}$ Figure 4: The SED for an impulsive MQ for R=10 pc at three different epochs: for 100 yr (curve 1); for 1000 yr (2); and for 10 000 yr (3). The photon energy axis units in this and following plots are m $_{\rm e}$ c².
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1794fig5.eps} \end{figure}$ Figure 5: The same as in Fig. 4 but for a continuous MQ (recall: t=100 yr (1); 1000 yr (2); and 10 000 yr (3)).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1794fig6.eps} \end{figure}$ Figure 6: a) SED from the galactic cosmic rays interacting with a cloud. The power-law index for proton energy distribution has been taken to be 2.75, as is found near the Earth. Diffusion does not depend on energy. b) SED from a continuous MQ: in one case the diffusion is energy dependent (solid line), in the other case it is not (long-dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1794fig7.eps} \end{figure}$ Figure 7: The SED for an impulsive MQ for t=1000 yr at three different R: for 100 pc (curve 1), for 30 pc (2), and for 10 pc (3).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1794fig8.eps} \end{figure}$ Figure 8: The same as in Fig. 7 but for a continuous MQ (recall: R=100 pc (1), 30 pc (2), and 10 pc (3)).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1794fig9.eps} \end{figure}$ Figure 9: SED of an impulsive MQ taking R=10 pc, t=100 yr, and two magnetic field strength B=10^-3 G (1) and 10^-5 G (2).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1794fig10.eps} \end{figure}$ Figure 10: The same as in Fig. 9, but for a t=10 000 yr (B=10^-3 G (1) and 10^-5 G (2)).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1794fig11.eps} \end{figure}$ Figure 11: SED of an impulsive source at R=10 pc after t=1000 yr. We have plotted both the cases for U=1 eV cm^-3 (1) and U=10 000 eV cm^-3 (2).
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{1794fig12.eps} \end{figure}$ Figure 12: SED of a complex source: a continuous MQ (long-dashed line) plus an impulsive phase (dotted line). t=10⁵ yr for the first one and t=200 yr for the second one, with R=10 pc. The added spectrum is presented as a thick solid line. The kinetic energy luminosity for the continuous MQ has been taken to be 10³⁷ erg s^-1, and the kinetic energy for the impulsive MQ has been taken to be 10⁴⁸ erg.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{1794fig13.eps} \end{figure}$ Figure 13: SED of the observed spectrum from two clouds interacting with an impulsive MQ at distances 5 and 50 pc.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{1794fig14.eps} \end{figure}$ Figure 14: SED of a continuous MQ at t =10⁶ yr and R=10 pc reproducing a typical GeV source (solid line). The value of the cloud mass is 10⁵ M $_{\odot }$ . An extrapolation of a typical EGRET spectrum up to $\sim$ 10 GeV is also shown (long-dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1794fig1.eps} \end{figure}$	Figure 1: Spectrum of protons released from a source at R=10 pc after t=100 yr (solid line) and 10 000 yr (long-dashed line). The dotted horizontal line shows the flux of cosmic ray protons observed near the Earth. a) For an impulsive MQ. b) For a continuous MQ.
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$\begin{figure} \includegraphics[width=8.6cm,clip]{1794fig2.eps} \end{figure}$	Figure 2: Proton and electron energy distributions (solid and long-dashed lines respectively) for an impulsive MQ at R=10 pc. The kinetic energy axis units are m $_{\rm e}$ c². a) The source age is t=100 yr. b) The source age is 1000 yr.
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$\begin{figure} \includegraphics[width=8.6cm,clip]{1794fig3.eps} \end{figure}$	Figure 3: The same as in Fig. 2 but for a continuous MQ (recall: a) t=100 yr; b) t=1000 yr).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1794fig4.eps} \end{figure}$	Figure 4: The SED for an impulsive MQ for R=10 pc at three different epochs: for 100 yr (curve 1); for 1000 yr (2); and for 10 000 yr (3). The photon energy axis units in this and following plots are m $_{\rm e}$ c².
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1794fig5.eps} \end{figure}$	Figure 5: The same as in Fig. 4 but for a continuous MQ (recall: t=100 yr (1); 1000 yr (2); and 10 000 yr (3)).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1794fig6.eps} \end{figure}$	Figure 6: a) SED from the galactic cosmic rays interacting with a cloud. The power-law index for proton energy distribution has been taken to be 2.75, as is found near the Earth. Diffusion does not depend on energy. b) SED from a continuous MQ: in one case the diffusion is energy dependent (solid line), in the other case it is not (long-dashed line).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1794fig7.eps} \end{figure}$	Figure 7: The SED for an impulsive MQ for t=1000 yr at three different R: for 100 pc (curve 1), for 30 pc (2), and for 10 pc (3).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1794fig8.eps} \end{figure}$	Figure 8: The same as in Fig. 7 but for a continuous MQ (recall: R=100 pc (1), 30 pc (2), and 10 pc (3)).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1794fig9.eps} \end{figure}$	Figure 9: SED of an impulsive MQ taking R=10 pc, t=100 yr, and two magnetic field strength B=10^-3 G (1) and 10^-5 G (2).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1794fig10.eps} \end{figure}$	Figure 10: The same as in Fig. 9, but for a t=10 000 yr (B=10^-3 G (1) and 10^-5 G (2)).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1794fig11.eps} \end{figure}$	Figure 11: SED of an impulsive source at R=10 pc after t=1000 yr. We have plotted both the cases for U=1 eV cm^-3 (1) and U=10 000 eV cm^-3 (2).
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{1794fig13.eps} \end{figure}$	Figure 13: SED of the observed spectrum from two clouds interacting with an impulsive MQ at distances 5 and 50 pc.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{1794fig14.eps} \end{figure}$	Figure 14: SED of a continuous MQ at t =10⁶ yr and R=10 pc reproducing a typical GeV source (solid line). The value of the cloud mass is 10⁵ M $_{\odot }$ . An extrapolation of a typical EGRET spectrum up to $\sim$ 10 GeV is also shown (long-dashed line).
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