  The interaction of escaping upper atmosphere of a hydrogen rich
non-magnetized analog of HD209458b with a stellar wind of its host G-type star
at different orbital distances is simulated with a 2D axisymmetric multi-fluid
hydrodynamic model. A realistic sun-like spectrum of XUV radiation which
ionizes and heats the planetary atmosphere, hydrogen photo-chemistry, as well
as stellar-planetary tidal interaction are taken into account to generate
self-consistently an atmospheric hydrodynamic outflow. Two different regimes of
the planetary and stellar winds interaction have been modelled. These are: 1)
the "captured by the star" regime, when the tidal force and pressure gradient
drive the planetary material beyond the Roche lobe towards the star, and 2) the
"blown by the wind" regime, when sufficiently strong stellar wind confines the
escaping planetary atmosphere and channels it into the tail. The model
simulates in details the hydrodynamic interaction between the planetary atoms,
protons and the stellar wind, as well as the production of energetic neutral
atoms (ENAs) around the planet due to charge-exchange between planetary atoms
and stellar protons. The revealed location and shape of the ENA cloud either as
a paraboloid shell between ionopause and bowshock (for the "blown by the wind"
regime), or a turbulent layer at the contact boundary between the planetary
stream and stellar wind (for the "captured by the star" regime) are of
importance for the interpretation of Ly{\alpha} absorption features in
exoplanetary transit spectra and characterization of the plasma environments.
