  We present a simple model in which the bullets that produce the "Orion
fingers" (ejected by the BN/KL object) are interpreted as protoplanets or low
mass protostars in orbit around a high mass star that has a supernova
explosion. As the remnant of the SN explosion has only a small fraction of the
mass of the pre-supernova star, the orbiting objects then move away in free
trajectories, preserving their orbital velocity at the time of release. We show
that a system of objects arranged in approximately co-planar orbits results in
trajectories with morphological and kinematical characteristics resembling the
Orion fingers. We show that, under the assumption of constant velocity motions,
the positions of the observed heads of the fingers can be used to reconstruct
the properties of the orbital structure from which they originated, resulting
in a compact disk with an outer radius of $\sim 2.4$~AU.
