All Figures

Figure 1: MECS background subtracted light curves of RX J1826.2-1450 in different energy ranges. Each point represents 60 min. Time zero corresponds to JD 2 451 825.75. The expected time of periastron (P) and inferior conjunction (IC) of the primary are indicated in the top panel, where the error bars represent the uncertainty in the zero point of the ephemeris. The time difference between these two points is  s. An estimate of the unabsorbed X-ray luminosity according to the model of Table 1 is also given in the right axis of the top panel.

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In the text

	Figure 2: LECS energy spectrum of RX J1826.2-1450 and the best-fit model displayed in Table 1.
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In the text

	Figure 3: MECS energy spectrum of RX J1826.2-1450 and the best-fit model displayed in Table 1.
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In the text

Figure 4: Expected variability of the X-ray luminosity in LS 5039 due to the significantly eccentric orbit of the compact companion around the O6.5V((f)) star with a period  d, using a spherically symmetrical Bondi-Hoyle accretion model and the parameters quoted in the text. The thick line corresponds to e=0.41, the nominal eccentricity value in the McSwain et al. (2001) solution, while the lower and upper thin lines are for e=0.36 and e=0.46, which correspond to the error limits quoted by the authors. Phase 0 corresponds to periastron, while the shaded areas correspond to the phase interval covered by our BeppoSAX observation.

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In the text