Mr José Carlos Jiménez Apaza (UFRJ)
The study of the inner structure of compact stars requires the knowledge of the equation of state (EoS) for this kind of exotic stellar matter. This show us how the balance between gravitational attraction and microscopic interaction by means of the other fundamental interactions gives rise to the state of equilibrium in which they are observed currently. In the case of quark or hybrid neutron stars, it is known that the strong interaction plays the dominant role. In principle one could ﬁnd the EoS for this kind of star matter using the fundamental equations of quantum chromodynamics (QCD). However, the non-perturbative regime of this theory is highly nontrivial and therefore one cannot ﬁnd an exact EoS for the interior of such stars that takes into account all the physical and mathematical structure of QCD. Up to now one is only able to solve the fundamental equations if one simpliﬁes QCD, keeping some relevant symmetries, in order to build eﬀective models. In this work we test some EoS’s, which were obtained by using approximate results from eﬀective models, by solving the Tolman-Oppenheimer-Volkoﬀ (TOV) equations in order to determine some important intrinsic properties of such exotic stars, like the mass-radius relation, etc.