Bochum 2009 – scientific programme

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HK: Fachverband Hadronen und Kerne

HK 73: Nuclear Astrophysics

HK 73.2: Talk

Thursday, March 19, 2009, 17:00–17:15, H-ZO 60

A Statistical Model for Supernova Matter — •Matthias Hempel¹ and Jürgen Schaffner-Bielich² — ¹Institut für Theoretische Physik, Goethe-Universität, Max-von-Laue-Str. 1, 60438 Frankfurt am Main, Germany — ²Institut für Theoretische Physik, Ruprecht-Karls-Universität, Philosophenweg 16, 69120 Heidelberg, Germany

The equation of state and the composition of hot hadronic matter is described by an ensemble of nuclei and interacting nucleons in nuclear statistical equilibrium. A relativistic mean field model is applied for the nucleons. The masses of the nuclei are taken from nuclear structure calculations which are based on the same nuclear Lagrangian. For known nuclei experimental data is used directly. To achieve a good description of the transition to uniform nuclear matter a thermodynamic consistent model is developed which implements excluded volume effects. The model is suitable for the entire range of conditions (T,n_B,Y_p) in core-collapse supernovae and a complete equation of state table is presented. Good agreement with other commonly used models based on the single nucleus approximation is found. Regarding the composition the importance of the statistical treatment and the nuclear distributions is illustrated. The role of shell effects is investigated. Special emphasis is put on the light clusters which are only poorly represented by alpha particles under certain conditions. As a first application the equation of state is used to study the evolution of cooling proto-neutron stars.