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We compare three different statistical models for the equation of state (EOS)of stellar matter at subnuclear densities and temperatures (0.5-10 MeV)expected to occur during the collapse of massive stars and supernovaexplosions. The models introduce the distributions of various nuclear speciesin nuclear statistical equilibrium, but use somewhat different nuclear physicsinputs. It is demonstrated that the basic thermodynamical quantities of stellarmatter under these conditions are similar, except in the region of highdensities and low temperatures. We demonstrate that mass and isotopicdistributions have considerable differences related to the differentassumptions of the models on properties of nuclei at these stellar conditions.Overall, the three models give similar trends, but the details reflect theuncertainties related to the modeling of medium effects, such as thetemperature and density dependence of surface and bulk energies of heavynuclei, and the nuclear shell structure effects. We discuss importance of newphysics inputs for astrophysical calculations from experimental data obtainedin intermediate energy heavy-ion collisions, in particular, the similarities ofthe conditions reached during supernova explosions and multifragmentationreactions.

A comparative study of statistical models for nuclear equation of state of stellar matter