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Generalized relativistic mean-field model with derivative nucleon-meson couplings for nuclear matter and finite nuclei

Sofija Antic (GSI, Darmstadt, Germany)

14h30 GANIL seminar room (105)

a coffee will be served 15mn before

The equation of state (EOS) for highly compressed dense matter is one  of the main concerns of nuclear astrophysics in recent years. It is essential for modeling compact astrophysical objects like neutron stars
(NS), their mergers and core collapse supernovae (CCSN). EOS also sets conditions for the creation of chemical elements in the universe, in particular for the r-process whose astrophysical site is still under
debate. Therefore, it is an active theoretical and experimental research topic.

  Since the realistic and quantitative description of dense matter is not available from first principles using the basic theory of quantum chromodynamics (QCD) a large variety of models is developed for this purpose. The phenomenological models depend on a number of adjustable parameters determined from observational and experimental data, which are essential for both nuclear structure and astrophysics applications. The characteristic saturation properties of nuclear matter and the density dependence of the effective interaction are usually addressed, while less attention is paid to its energy or momentum dependence. In this work the density dependent (DD) relativistic mean-field model (RMF) is generalized by introducing the energy dependence in the nucleon self-energies in order to reproduce the experimental behavior of the optical potential. The consequences are  studied for different nuclear systems, both for high and low density regions and for T = 0 and finite temperatures. The major impact of the additional energy dependence on the EOS stiffness, and therefore on the M-S relation for NS, implies the significance of the optical potential constraint. The main advantage of the model is its flexibility and the wide range of possible applications, from which several will be addressed.

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