Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{aa9252fig1.eps}\end{figure}$ Figure 1: Sketch of the physical scenario considered here. The long-dashed lines represent the wind, the straight dashed lines the secondary pair radiation, the straight solid lines the primary gamma rays, and the curved solid lines the advected/diffusing secondary pairs.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{aa9252fig2.eps}\end{figure}$ Figure 2: Upper panel: total $Q_{\rm int}~\gamma^2$ (solid line). $Q_{\rm int}~\gamma^2$ for R< d_* (long-dashed line) and >d_* (dotted line) are also shown. We adopt $\Gamma =2$ . Lower panel: total $N_{\rm int}~\gamma^2$ (solid line). $N_{\rm int}~\gamma^2$ for R< d_* (long-dashed line) and >d_* (dotted line) are also shown. We adopt $\Gamma =2$ , and B₀=1 (thin lines) and 100 G (thick lines). The dominant cooling mechanisms at different energies are given.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{aa9252fig3.eps}\end{figure}$ Figure 3: The same as in Fig. 2 but for $\Gamma =3$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{aa9252fig4.eps}\end{figure}$ Figure 4: The R-distribution of accumulated energy in secondary pairs (long-dashed line) and the R-distribution of accumulated energy rate via pair creation (dotted line) are shown. The location of the emitter is marked by a vertical thick dot-dashed line, at $\log(d_*)$ . In the plot, the star location would be at the left.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{aa9252fig5.eps}\end{figure}$ Figure 5: Upper panel: computed SEDs for the synchrotron and the IC secondary pair emission. We adopt B₀=100 G and $\Gamma =2$ . The emission from the whole volume (solid line) filled by particles, and that of a region located at $R<d_* - \sim 0.1$ mas at 3 kpc- (long-dashed line) and >d_* (dotted line). Lower panel: the same as the upper panel but for $\Gamma =3$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{aa9252fig6.eps}\end{figure}$ Figure 6: Upper panel: computed SEDs for the synchrotron and the IC secondary pair emission. We adopt B₀=1 (dotted line), 10 (long-dashed line) and 100 G (solid line), and $\Gamma =2$ . Lower panel: the same as the upper panel but for $\Gamma =3$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{aa9252fig7.eps}\end{figure}$ Figure 7: Upper panel: computed SEDs for the synchrotron and the IC secondary pair emission produced in the whole volume (solid line) and the region beyond >d_* (long dashed). We adopt B₀=100 G and $\Gamma =2.5$ . Lower panel, left: radio SEDs for different regions: R< 1 (long dashed), >1 (solid line), >2 (dotted line) and >3 AU (dot-dashed line). Lower panel, right: spatial distribution of the emitting particles, for the orbital plane (a) and a plane perpendicular to it (b), in the surroundings of LS I +61 303 after one orbital period. The star is centered on the origin. We note that the system size is $\approx$ 0.4 AU, and $1~{\rm AU}\approx 0.5$ milliarcsec.
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{aa9252fig8.eps}\end{figure}$ Figure A.1: Geometry of the photon-photon interaction.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{aa9252fig1.eps}\end{figure}$	Figure 1: Sketch of the physical scenario considered here. The long-dashed lines represent the wind, the straight dashed lines the secondary pair radiation, the straight solid lines the primary gamma rays, and the curved solid lines the advected/diffusing secondary pairs.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{aa9252fig3.eps}\end{figure}$	Figure 3: The same as in Fig. 2 but for $\Gamma =3$ .
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{aa9252fig4.eps}\end{figure}$	Figure 4: The R-distribution of accumulated energy in secondary pairs (long-dashed line) and the R-distribution of accumulated energy rate via pair creation (dotted line) are shown. The location of the emitter is marked by a vertical thick dot-dashed line, at $\log(d_*)$ . In the plot, the star location would be at the left.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{aa9252fig5.eps}\end{figure}$	Figure 5: Upper panel: computed SEDs for the synchrotron and the IC secondary pair emission. We adopt B₀=100 G and $\Gamma =2$ . The emission from the whole volume (solid line) filled by particles, and that of a region located at $R<d_* - \sim 0.1$ mas at 3 kpc- (long-dashed line) and >d_* (dotted line). Lower panel: the same as the upper panel but for $\Gamma =3$ .
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{aa9252fig6.eps}\end{figure}$	Figure 6: Upper panel: computed SEDs for the synchrotron and the IC secondary pair emission. We adopt B₀=1 (dotted line), 10 (long-dashed line) and 100 G (solid line), and $\Gamma =2$ . Lower panel: the same as the upper panel but for $\Gamma =3$ .
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$\begin{figure} \par\includegraphics[width=6.4cm,clip]{aa9252fig8.eps}\end{figure}$	Figure A.1: Geometry of the photon-photon interaction.
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