Dynamics of few‐body states in a medium
Strongly interacting matter such as nuclear or quark matter leads to few‐body bound states and correlations of the constituents. As a consequence quantum chromodynamics has a rich phase structure with spontaneous symmetry breaking, superconductivity, condensates of different kinds. All this appears in many astrophysical scenarios. Among them is the formation of hadrons during the early stage of the Universe, the structure of a neutron star, and the formation of nuclei during a supernova explosion. Some of these extreme conditions can be simulated in heavy ion colliders. To treat such a hot and dense system we use the Green function formalism of many‐body theory. It turns out that asystematic Dyson expansion of the Green functions leads to modified few‐body equations that are capable to describe phase transitions, condensates, cluster formation and more. These equations include self energy corrections and Pauli blocking. We apply this method to nonrelativistic and relativistic matter. The latter one is tre...