Quark-gluon plasma and transition to hadrons at nucleation in astrophysics plasmas at Boltzmann equilibrium

![CDATA[One key problem in astrophysics is to explain how the elements above iron are created. Based on the key role in the transition of the Fermi statistics for hadrons changing from the relativistic branch into the subrelativistic branch the stable configuration for the nuclei just at the well-known density of nuclei was calculated. If the transition of higher than nuclear density at the big bang or at expansion of neutron stars e.g. in a supernova appears under Boltzmann equilibrium, the nucleation including the heavy elements leads to a relation of the magic numbers explaining the transition in the Bagge series. An understanding is derived why then only the elements up to about uranium appear and that the elements above curium are typical manmade non-equilibrium creations. This is based on the experimental facts on the standard abundance distribution (SAD) in the Universe, and the Boltzmann relation.]]