  Signatures of "evaporative" winds from exo-planets on short (hot) orbits
around their host star have been observed in a number of systems. In this paper
we present global AMR simulations that track the launching of the winds, their
expansion through the circumstellar environment, and their interaction with a
stellar wind. We focus on purely hydrodynamic flows including the anisotropy of
the wind launching and explore the orbital/fluid dynamics of the resulting
flows in detail. In particular we find that a combination of the tidal and
Coriolis forces strongly distorts the planetary "Parker" wind creating
"up-orbit" and "down-orbit" streams. We characterize the flows in terms of
their orbital elements which change depending on their launch position on the
planet. We find that the anisotropy in the atmospheric temperature leads to
significant backflow on to the planet. The planetary wind interacts strongly
with the stellar wind creating instabilities that cause eventual deposition of
planetary gas onto the star. We present synthetic observations of both transit
and absorption line-structure for our simulations. For our initial conditions,
we find that the orbiting wind material produces absorption signatures at
significant distances from the planet and substantial orbit to orbit
variability. Ly-{\alpha} absorption shows red and blueshifted features out to
70 km/s. Finally, using semi-analytic models we constrain the effect of
radiation pressure, given the approximation of uniform stellar absorption.
