  The origin of the orbital structure of the cold component of the Kuiper belt
is still a hot subject of investigation. Several features of the solar system
suggest that the giant planets underwent a phase of global dynamical
instability, but the actual dynamical evolution of the planets during the
instability is still debated. To explain the structure of the cold Kuiper belt,
Nesvorny (2015, AJ 150,68) argued for a soft instability, during which Neptune
never achieved a very eccentric orbit. Here we investigate the possibility of a
more violent instability, from an initially more compact fully resonant
configuration of 5 giant planets. We show that the orbital structure of the
cold Kuiper belt can be reproduced quite well provided that the cold population
formed in situ, with an outer edge between 44 and 45 au and never had a large
mass.
