  We use radiation hydrodynamics with direct particle integration to explore
the feasibility of chondrule formation in planetary embryo bow shocks. The
calculations presented here are used to explore the consequences of a Mars-size
planetary embryo traveling on a moderately excited orbit through the dusty,
early environment of the solar system. The embryo's eccentric orbit produces a
range of supersonic relative velocities between the embryo and the circularly
orbiting gas and dust, prompting the formation of bow shocks. Temporary
atmospheres around these embryos, which can be created via volatile outgassing
and gas capture from the surrounding nebula, can non-trivially affect thermal
profiles of solids entering the shock. We explore the thermal environment of
solids that traverse the bow shock at different impact radii, the effects that
planetoid atmospheres have on shock morphologies, and the stripping efficiency
of planetoidal atmospheres in the presence of high relative winds. Simulations
are run using adiabatic and radiative conditions, with multiple treatments for
the local opacities. Shock speeds of 5, 6, and 7 km/s are explored. We find
that a high-mass atmosphere and inefficient radiative conditions can produce
peak temperatures and cooling rates that are consistent with the constraints
set by chondrule furnace studies. For most conditions, the derived cooling
rates are potentially too high to be consistent with chondrule formation.
