All Figures

	Figure 1: Accretion curve along an orbital period inferred from the observed X-ray lightcurve in Bosch-Ramon et al. (2005a), adopting the accretion model developed for this work.
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In the text

	Figure 2: The photon absorption coefficient as a function of the energy for photons emitted in the jet at different distances from the compact object, at periastron and apastron passages.
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In the text

Figure 3: Comparison of the spectral energy distribution of LS 5039 computed from the present model, at the periastron passage and using the parameters of Table 1, with the observed data. We show the different components of the emission as well as the sum of all of the them, which is attenuated due to absorption (solid line). The points observed are from Martí et al. (1998) (VLA, diamond), Clark et al. (2001) and Drilling (1991) (optical, circle, corrected of absorption), Bosch-Ramon et al. (2005a) (RXTE, square), Harmon et al. (2004) (BATSE, diamond filled), Collmar et al. (2003) (COMPTEL, square filled), Hartman et al. (1999) (EGRET, circle filled) and Aharonian et al. (2005a) (HESS, triangle down filled). The arrows in the EGRET and HESS data represent upper limits (3).

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In the text

	Figure 4: The panel shows the flux variations along the orbit for the four energy bands considered here. We note that emission at very high-energy -rays is strongly attenuated by the photon absorption in the star photon field.
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In the text