  We preform hybrid simulations of super Alfvenic quasi-parallel shock, driven
by a Coronal Mass Ejection (CME), propagating in the Outer Coronal or Solar
Wind at distances of between 3 to 6 solar radii. The hybrid treatment of the
problem enable the study of the shock propagation on the ion time scale,
preserving ion kinetics and allowing for a self consistent treatment of the
shock propagation and particle acceleration. The CME plasma drags the embedded
magnetic field lines stretching from the sun, and propagates out into
interplanetary space at a greater velocity than the in-situ solar wind, driving
the shock, and producing very energetic particles. Our results show
electromagnetic Alfven waves are generated at the shock front. The waves
propagate upstream of the shock and are produced by the counter streaming ions
of the solar wind plasma being reflected at the shock. A significant fraction
of the particles are accelerated in two distinct phases: first, particles drift
from the shock and are accelerated in the upstream region and, second,
particles arriving at the shock get trapped, and are accelerated at the shock
front. A fraction of the particles diffused back to the shock, which is
consistent with the Fermi acceleration mechanism.
