Shun Furasawa, NAOJ, Japan
Hot and dense matter can be realised in core collapse supernovae and mergers of compact stars. The mechanisms of those explosive events are not clearly understood yet because of their intricacies. One of the underlying problems is related to uncertainties in input physics, such as the equation of state of hot and dense stellar matter. In this talk I will give a short overview about the equations of state used in such simulations. Then I will present a new approach, in which the properties of individual nuclei (equilibrium densities and binding energies) are calculated self-consistently with their abundencies in the nuclear ensemble. In particular, I will demonstrate that heavy nuclei in the ensemble are either compressed or decompressed depending on the isospin asymmetry of the system.