Effects of the temperature dependence of the in-medium nucleon mass on core-collapse supernovae
1 Institut d’Astronomie et d’Astrophysique, CP226, Université Libre de Bruxelles, 1050 Brussels, Belgium
2 CEA, DAM, DIF, 91297 Arpajon, France
3 Laboratoire Univers et Théories, Observatoire de Paris, CNRS, 92190 Meudon, France
4 Institut de Physique Nucléaire, Université Paris-Sud, IN2P3-CNRS, 91406 Orsay Cedex, France
5 Dipartimento di Fisica, Università degli Studi di Milano, and Istituto Nazionale di Fisica Nucleare, Sezione di Milano, via Celoria 16, 20133 Milano, Italy
Received: 30 September 2011
Accepted: 3 February 2012
Aims. A complete description of the core collapse supernova mechanism requires an appropriate treatment of both the hydrodynamics and the microphysics. We study the influence of a nuclear physics input, namely the temperature dependence of the nucleon effective mass in nuclei induced by the in-medium effects, in the core collapse of a massive star.
Methods. We present here the first implementation of this nuclear input in a hydrodynamical one-dimensional simulation. The simulations are performed with a spherically symmetric Newtonian model, with neutrino transport treated in the multi-group flux-limited diffusion approximation.
Results. The inclusion of the temperature dependence of the in-medium nucleon mass has an impact on the equation of state of the system and reduces the deleptonisation during the collapse. This results in a non-negligible effect on the shock wave energetics. The shock wave is formed more outwards, and in the first few milliseconds after bounce the shock front has propagated further out.
Key words: equation of state / methods: numerical / hydrodynamics / supernovae: general
© ESO, 2012