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The crust-core transition and the stellar matter equation of state

Helena Pais (CFisUC, Department of Physics, University of Coimbra, Portugal)

11h00 GANIL seminar room (105)

a coffee will be served 15mn before


Neutron stars are one of the most dense objects in the Universe. In this talk, we will start by giving a brief introduction to these compact objects. Our goal is to describe the macroscopic properties of the star, that is, its mass and radius. For that, we will need first to construct the stellar matter equation of state (EoS), which should be in accordance with constrains coming from both observations and experiments. We will use two different formalisms for the EoS, relativistic mean-field models and the SU(2) extended Nambu–Jona-Lasinio. Quantities like the crust-core transition density and pressure, will be introduced, and their effect on the mass-radius relation of the star will be discussed. The effect on the star radius of the inclusion of a pasta calculation in the inner crust is also discussed, for all the models considered. Finally, we will show the effect of strong external magnetic fields on the inner crust of the star. This is of the utmost importance for the study of magnetars, neutron stars with very strong magnetic fields, which have yet to be understood in more detail.

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