Köln 2025 – scientific programme
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HK: Fachverband Physik der Hadronen und Kerne
HK 32: Nuclear Astrophysics IV
HK 32.2: Talk
Wednesday, March 12, 2025, 16:15–16:30, SR 0.03 Erw. Physik
Equation of state effects in core-collapse supernova simulations — •Finia P. Jost1, Andre da Silva Schneider2, Gerard Navo3, Yeunhwan Lim4, Sabrina Huth1, Almudena Arcones1,5,6, and Achim Schwenk1,6 — 1Institut für Kernphysik, Technische Universität Darmstadt, Darmstadt, Germany — 2Departamento de Física, Universidade Federal de Santa Catarina, Florianópolis, Brazil — 3Departament d'Astronomia i Astrofisica, Universitat de Valencia, Valencia, Spain — 4Department of Physics, Yonsei University, Seoul, South Korea — 5GSI Helmholtzzentrum fuer Schwerionenforschung GmbH, Darmstadt, Germany — 6Max-Planck-Institut fuer Kernphysik, Heidelberg, Germany
The equation of state (EOS) of dense matter remains uncertain, especially at higher densities. The dynamics of core-collapse supernovae and the properties of newly formed proto-neutron stars directly depend on the state of matter at these high densities. We provide new EOS tables based on the EOS models of Huth et al. 2021 covering the necessary range in density, temperature, and electron fraction to be used in astrophysical simulations. The EOS are consistent with all currently available constraints from theoretical and experimental nuclear physics as well as observations of neutron stars. We systematically vary cold nuclear matter properties within their uncertainties and explore their impact in simulations of core-collapse supernovae. Additionally, we explore the impact of the new prescription of the density-dependent effective mass of nucleons, which governs the thermal nucleonic contribution to the EOS.
Keywords: Nuclear Equation of State; Core-collapse Supernovae