  The absorption of stellar radiation observed by the HD209458b in resonant
lines of OI and CII has not yet been satisfactorily modeled. In our previous 2D
simulations we have shown that the hydrogen-dominated upper atmosphere of
HD209458b, heated by XUV radiation, expands supersonically beyond the Roche
lobe and drags the heavier species along with it. Assuming solar abundances, OI
and CII particles accelerated by tidal forces to velocities up to 50 km/s
should produce the absorption due to Doppler resonance mechanism at the level
of 6-10%, consistent with the observations. Since the 2D geometry does not take
into account the Coriolis force in the planet reference frame, the question
remained to which extent the spiraling of the escaping planetary material and
its actually achieved velocity may influence the conclusions made on the basis
of 2D modeling. In the present paper we apply for the first time in the study
of HD209458b a global 3D hydrodynamic multi-fluid model that self-consistently
describes the formation and expansion of the escaping planetary wind, affected
by the tidal and Coriolis forces, as well as by the surrounding stellar wind.
The modeling results confirm our previous findings that the velocity and
density of the planetary flow are sufficiently high to produce the absorption
in HI, OI, and CII resonant lines at the level close to the in-transit observed
values. The novel finding is that the matching of the absorption measured in
MgII and SiIII lines requires at least 10 times lower abundances of these
elements than the Solar system values.
