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$\begin{figure} \par\includegraphics[width=8cm,clip]{5240fig1.eps}\end{figure}$ Figure 1: Microquasars (position and type) in the Galaxy.
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In the text

$\begin{figure} \par\includegraphics[width=9.0cm,clip]{5240fig2.eps}\end{figure}$ Figure 2: Schematic view of the irradiation of the secondary star by a jet. The binary system frame is represented by the dashed axes.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5240fig3.eps}\end{figure}$ Figure 3: Instantaneous 511 keV photon flux induced by the jet (red curve) and the counterjet (blue curve) impacts on the secondary of a virtual XRB (see text). The jet inclination with respect to the binary plane is taken to be $i_{{\rm jet}}$ = 9 $^{\circ }$ , its opening angle is $\theta _{{\rm jet}}$ = 1 $^{\circ }$ ; the precession period is 300 days (see text). The positron rate and energy in each jet is ${\dot N}_{{\rm e}^+} = 10 ^{41}$ s^-1 and E = 660 keV ( $v_{{\rm jet}} = 0.9$ c), respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5240fig4.eps}\end{figure}$ Figure 4: Details of the instantaneous 511 keV photon flux induced by the jet (red curve) and the counterjet (blue curve) impacts on the secondary of a virtual XRB (see caption of Fig. 3). a) The jet direction is parallel to the observer direction and only the hotspot induced by the first jet is visible; b) the jet direction is perpendicular to the observer direction and both hotspots induced by the jet and the counterjet are visible. The geometrical configurations of the jets and the binary system in these two cases are shown in Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5240fig5.eps}\end{figure}$ Figure 5: Schematic views of the jets (blue) arising from the compact object (black), the secondary star (red) presented at four positions in its orbit, and the annihilation hotspot (yellow) emitted from the secondary star atmosphere, presented at the dates $\sim$ 2 days a) and $\sim$ 75 days b). The directions of motion of the secondary star and jets axis are represented by arrows. The two configurations correspond approximately to the cases a and b of Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5240fig6.eps}\end{figure}$ Figure 6: Average 511 keV photon flux per XRB period, induced by the jet impacts on the secondary of an XRB. The parameters of the jets are identical to those of Figure.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5240fig7.eps}\end{figure}$ Figure 7: Spectra of the annihilation radiation emitted by GRO J1655-40. The parameters of the jets are identical to those of Fig. 3. We assumed that the 50% of positrons annihilates with the ionized component of the atmosphere and 50% with the neutral component. Case 1: total spectrum integrated over the precession period; case 2: spectrum integrated over one period at the date 100 days; case 3: spectrum integrated over one period at the date 200 days.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5240fig1.eps}\end{figure}$	Figure 1: Microquasars (position and type) in the Galaxy.
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$\begin{figure} \par\includegraphics[width=9.0cm,clip]{5240fig2.eps}\end{figure}$	Figure 2: Schematic view of the irradiation of the secondary star by a jet. The binary system frame is represented by the dashed axes.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{5240fig6.eps}\end{figure}$	Figure 6: Average 511 keV photon flux per XRB period, induced by the jet impacts on the secondary of an XRB. The parameters of the jets are identical to those of Figure.
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