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The physics of neutron stars leads historically towards Landau's speculation.Even before the discovery of the neutron, he postulated the possible existenceof stars more compact than white dwarfs, containing matter of the order ofnuclear density. From a modern point of view neutron stars are compact objectsmaintained by the equilibrium between gravity and the degeneracy pressure ofthe fermions together with a strong nuclear repulsion force due to the highdensity reached in their interior. While the physics in the vicinity of nuclearsaturation density is well know from phenomenology, the physics of ultra-densenuclear matter is still an open puzzle. In this work we study dense nuclearmatter within a relativistic model, allowing hyperons to be present throughbeta equilibrium. The presence of hyperons is justifiable since theconstituents of neutron stars are fermions. So, according to the Pauliprinciple, as the baryon density increases, so do the Fermi momentum and theFermi energy. On the other hand, this hyperonic matter softens the equation ofstate (EoS) and a recent measurement of pulsar PSR J1614-2230 implies that theEoS has to be stiff enough to produce a 2.0 $M_{\odot}$ pulsar. We alsoconsider Duncan's magnetar ideas and study the influence of strong magneticfields on the EoS. We see that a strong magnetic field produces very massiveneutron stars, in agreement with the astronomical observations.

The influence of Strong Magnetic Field in Hyperonic Neutron Stars