  We propose that the nebular shocks currently favored as a model to form
chondrules and other annealed silicates in the solar nebula originate in the
dynamical activity present in the envelope of forming Jovian planets. In
contrast to the classic `core accretion model', our 3D hydrodynamic simulations
show that this envelope is not a 1D hydrostatic structure but is instead
vigorously active and contains densities and temperatures that appear similar
in magnitude and spatial extent to those thought to be responsible for the
production of chondrules.
