Abstract
Correlations are an essential feature of interacting many-body systems such as nuclear and stellar matter. They cause the formation of clusters, i.e. nuclei and scattering resonances, changing the chemical composition and affecting the thermodynamical properties of the system. The equation of state has to be known in a wide range of density, temperature and isospin asymmetry for astrophysical simulations of core-collapse supernovae and compact stars. In a generalized relativistic density functional approach, the properties of dense stellar matter can be described with the correct limits at low densities, the model-independent virial equation of state, and at high densities using a quasiparticle mean-field approach. Effects of correlations and changes of the cluster properties in dilute matter can be studied experimentally in heavy-ion collisions.
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