  Context: Physics behind the soft X-ray light curve asymmetries in Cygnus X-3,
a well-known microquasar, was studied. AIMS: Observable effects of the jet
close to the line-of-sight were investigated and interpreted within the frame
of light curve physics. METHODS: The path of a hypothetical imprint of the jet,
advected by the WR-wind, was computed and its crossing with the line-of-sight
during the binary orbit determined. We explore the possibility that physically
this 'imprint' is a formation of dense clumps triggered by jet bow shocks in
the wind ("clumpy trail"). Models for X-ray continuum and emission line light
curves were constructed using two absorbers: mass columns along the
line-of-sight of i) the WR wind and ii) the clumpy trail, as seen from the
compact star. These model light curves were compared with the observed ones
from the RXTE/ASM (continuum) and Chandra/HETG (emission lines). Results: We
show that the shapes of the Cygnus X-3 light curves can be explained by the two
absorbers using the inclination and true anomaly angles of the jet as derived
in Dubus et al. (2010) from gamma-ray Fermi/LAT observations. The clumpy trail
absorber is much larger for the lines than for the continuum. We suggest that
the clumpy trail is a mixture of equilibrium and hot (shock heated) clumps.
Conclusions: A possible way for studying jets in binary stars when the jet axis
and the line-of-sight are close to each other is demonstrated. The X-ray
continuum and emission line light curves of Cygnus X-3 can be explained by two
absorbers: the WR companion wind plus an absorber lying in the jet path (clumpy
trail). We propose that the clumpy trail absorber is due to dense clumps
triggered by jet bow shocks.
